NAMERADECLIIBIIROLL_ANGLETIMESTOP_TIMEOBSIDEXPOSURETIME_AWARDEDXIS0_EXPOXIS1_EXPOXIS2_EXPOXIS3_EXPOXIS0_NUM_MODESXIS1_NUM_MODESXIS2_NUM_MODESXIS3_NUM_MODESHXD_NUM_MODESHXD_EXPO_COHXD_EXPO_FIHXD_EXPO_NOHXD_EXPOHXD_EXPO_WAMHXD_BURSTSPROCESSING_STATUSPROCESSING_DATEPUBLIC_DATEDISTRIBUTION_DATEPROCESSING_VERSIONNUM_PROCESSEDSOFTWARE_VERSIONPRNBABSTRACTSUBJECT_CATEGORYCATEGORY_CODEPRIORITYPI_LNAMEPI_FNAMECOPI_LNAMECOPI_FNAMECOUNTRYCYCLEOBS_TYPETITLEAIMPOINTINJECTION
E0102-7216.139-72.1205301.50933431-44.97149935119.406453593.308645833353595.24850694441000010102406.8700002406.82406.82406.82406.811110000000PROCESSED57520.68432870375424754035.59251157413.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000001XIS door open with a SMC SNR E0102-72CALIBRATION1ASWGNULLNULLNULLJAP0SWGXIS door openNULLN
E0102-7215.9884-72.0403301.56673438-45.05476105119.551253595.248923611153595.46185185181000010204159.8100004159.84159.84159.84159.811120000000PROCESSED57520.67798611115424754035.63127314823.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000001XIS door open with a SMC SNR E0102-72CALIBRATION1ASWGNULLNULLNULLJAP0SWGXIS door openNULLN
N132D81.2794-69.6524280.31514531-32.7756605153.329153595.470312553597.53135416671000020107406.6800007406.67406.67406.67406.622220000000PROCESSED57520.71096064825424754038.58759259263.0.22.436Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000002HXD HV ON WITH N132D, and 5 pointings with XISCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD HV ON WITH N132DNULLN
N132D81.1356-69.5861280.24807804-32.8367013553.463953597.531736111153597.693229166710000202007000000000000000000PROCESSED57520.67688657415424754230.41318287043.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000002HXD HV ON WITH N132D, and 5 pointings with XISCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD HV ON WITH N132DNULLN
N132D81.4173-69.7177280.38157857-32.7170587453.19853597.693981481553597.836932870410000203007000000000000000000PROCESSED57520.68252314825424754230.41334490743.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000002HXD HV ON WITH N132D, and 5 pointings with XISCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD HV ON WITH N132DNULLN
N132D81.0865-69.7023280.38777612-32.8326824953.511853597.837553597.986562510000204007000000000000000000PROCESSED57520.68402777785424754230.41487268523.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000002HXD HV ON WITH N132D, and 5 pointings with XISCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD HV ON WITH N132DNULLN
N132D81.4727-69.6025280.24276086-32.7181120253.148553597.986944444453598.239895833310000205007000000000000000000PROCESSED57520.68732638895424754230.41572916673.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000002HXD HV ON WITH N132D, and 5 pointings with XISCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD HV ON WITH N132DNULLN
N132D81.2751-69.6506280.31335191-32.7774499453.331253598.240277777853598.51400462961000020605963.570005963.55963.55963.55963.511110000000PROCESSED57520.69251157415424754038.47008101853.0.22.436Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000002HXD HV ON WITH N132D, and 5 pointings with XISCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD HV ON WITH N132DNULLN
DEM_L71/N2376.4474-67.958278.75859594-34.8358188570.584953598.520636574153599.60425925931000030105789.7400005789.75789.75789.75789.722220000093606.10PROCESSED57520.70986111115424754035.70181712963.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000003LMC SNRs L71/N23CALIBRATION1ASWGNULLNULLNULLJAP0SWGLMC SNRsNULLN
MCG-6-30-15203.9795-34.2919313.2980527327.68293005295.97153599.673530092653601.145902777810000401046698.74000046700.950916.946698.746725.4333310046484.646484.6127099.90PROCESSED57520.73263888895424754035.79917824073.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000004NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGMCG-60-30-15NULLN
Cen A201.3695-43.0177309.5195082919.41821819303.915853601.152303240753602.409814814810000501064675.94000064694.264765.864675.964739.9525510066258.266258.2108611.90PROCESSED57520.73619212965370553905.45971064823.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000005NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGCen ANULLN
A 2052229.27796.87669.3133991949.96215441281.232853602.423807870453602.74328703710000601013902.12000013902.113902.113902.113902.1111110013416.313416.327583.90PROCESSED57520.72074074075370553905.46075231483.0.22.4311Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000006NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGOuter region of A 2052NULLN
A 2052229.32377.10599.6471147150.05514889281.237353602.744039351853603.340694444510000602025743.12000025743.125743.125743.125743.1111110021064.221064.251519.90PROCESSED57520.72465277785370553905.46103009263.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000006NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGOuter region of A 2052NULLN
A 2052229.09337.15169.5033552750.26933049281.209353603.341261574153603.6114351852100006030129692000012969129691296912969111110013141.313141.323327.90PROCESSED57520.72715277785370553905.46133101853.0.22.439Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000006NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGOuter region of A 2052NULLN
A 2052229.04716.92119.1664668950.17566284281.203153603.612187553603.993842592610000604016744.32000016744.316744.316744.316744.3111110012839.512839.532951.90PROCESSED57520.73258101855370553905.46341435183.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000006NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGOuter region of A 2052NULLN
A 2052229.33117.26329.8557914350.1380787791.237153762.48265046353762.92099537041000060502236620000223662236622366223662222100203882038837865.90PROCESSED57532.8001620375424754040.53186342593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000006NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGOuter region of A 2052XISN
Crab Nebula83.627422.0192184.55062413-5.7862938586.866353604.157141203753604.25012731481000070101722.950001722.91722.91722.91722.911111001808180880340PROCESSED57520.73303240745424754105.27589120373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000007Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab NebulaNULLN
Crab nebula83.620122.1854184.40591259-5.7030077686.863153604.250717592653604.38893518521000070203053.150003057.13053.13053.13053.111111003134.33134.3119401PROCESSED57520.74167824075424754105.29872685183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000007Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab NebulaNULLN
Crab nebula83.639921.8519184.69891686-5.8660409986.868353604.389826388953604.48909722221000070302786.150002786.12786.12790.12786.111111002192.72192.78554.10PROCESSED57520.74162037045424754105.28653935183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000007Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab NebulaNULLN
Crab nebula83.451222.0082184.47195778-5.9301048686.798953604.48984953753604.58354166671000070404268.250004268.24268.24268.24268.211111004139.24139.280560PROCESSED57520.74545138895424754105.30737268523.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000007Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab NebulaNULLN
Crab nebula83.808322.0272184.63396429-5.6403124386.934253604.584479166753604.647986111110000705032625000326232623262326211111003179317954480PROCESSED57520.74905092595424754105.33341435183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000007Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab NebulaNULLN
NGC 4945196.3712-49.4666305.2766379313.34118784313.906253604.778831018553605.1010763889100008010143381500014338143381433814338222210013806.713806.727841.91PROCESSED57526.85538194445424754035.52121527783.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000008NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGNGC 4945NULLN
NGC 4945196.3733-49.4666305.2780383513.34111135313.907853605.10108796353605.1034490741100008020177.610000181.5181.5179.6177.61111100200.1200.12020PROCESSED57526.84865740745424754034.68914351853.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000008NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGNGC 4945NULLN
NGC 4945196.3681-49.4152305.2775282713.3926200596.129653750.336562553752.965509259310000803095066.31000095081.795129.795066.395106.3222210084981.384981.3227115.72PROCESSED57532.73532407415424754040.35876157413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000008NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGNGC 4945HXDN
PSR1509-58228.4798-59.0943320.34145971-1.12587132287.634253605.3653606.859756944410000901065161.86000065161.865322.765242.765242.7333310049735.749735.7129529.84PROCESSED57526.90454861115370553905.46223379633.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000009HXD spectrum and timing checkCALIBRATION1ASWGNULLNULLNULLJAP0SWGPSR1509-58NULLN
Crab Nebula83.626722.0751184.50282132-5.7569130586.865553607.007083333353607.13898148151000100102937.950002937.92937.92937.92937.922221003438.73438.711381.90PROCESSED57526.86787037045424754118.98866898153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.633621.9568184.60669551-5.8148407586.868753607.139456018553607.27792824071000100203653.350003653.33653.33653.33653.311111003806.73806.7119340PROCESSED57526.87723379635424754118.93376157413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.610522.3483184.26290563-5.6232362586.859653607.279050925953607.51395833331000100308112.950008112.98112.98112.98112.922221007835.97835.9202641PROCESSED57526.88763888895424754118.96989583333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.651121.6763184.85366771-5.9511850586.879553607.515312553607.71534722221000100409580.650009580.69580.69580.69580.611111008178.38178.3172480PROCESSED57526.89818287045424754118.9431253.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.270821.9976184.39063256-6.0768938586.733153607.716516203753607.91673611111000100509346.950009346.99346.99346.99346.911111006653665317287.90PROCESSED57526.95424754122.42236111113.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.567722.0135184.52566905-5.8360869586.844453607.917581018553608.06950231481000100604877.950004877.94877.94877.94877.911111005021.75021.7130760PROCESSED57526.90660879635424754122.41954861113.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.692222.0221184.58047361-5.7339953886.867153608.069976851853608.20840277781000100704089.950004089.94089.94089.94089.911111004228.34228.311925.90PROCESSED57526.90722222225424754119.01490740743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.622222.1365184.44846107-5.7275551286.866653608.208923611153608.31608796310001008033825000338233823382338211111003700.33700.39253.90PROCESSED57526.91408564825424754119.00561342593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.580722.8483183.82410841-5.3783209986.867753608.317581018553608.513958333310001009067165000671667166716671611111006376.86376.816950.10PROCESSED57526.91646990745424754119.02356481483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.988722.0345184.71743044-5.4949944186.866653608.515590277853608.715347222210001010096945000969496949694969411111007581.27581.217247.90PROCESSED57526.92596064825424754122.42429398153.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.512224.0135182.80375415-4.8049732286.867553608.717997685253608.9306251000101109480.550009480.59480.59480.59480.5111110073637363183360PROCESSED57526.92651620375424754118.986253.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.637421.9009184.65605757-5.8417804986.866453608.933321759353609.0695254631000101204745.650004745.64745.64745.64745.622221005178.75178.711757.91PROCESSED57526.93432870375424754118.99461805563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.504422.0116184.49566519-5.8866513686.865853609.070138888953609.201458333310001013042225000422242224222422211111004372.44372.411335.90PROCESSED57526.93461805565424754119.04542824073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Crab nebula83.755222.0249184.60948321-5.6831474986.865653609.202210648253609.312581018510001014034195000341934193419341911111003755.43755.49531.90PROCESSED57526.93832175935424754118.99837962963.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000010Crab nebula multi pointingsCALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab Offset 1NULLN
Galactic bulge236.4313-31.7013340.9999453317.99808229283.544653609.436585648253611.060625100011010611337000061133611336113361133111110047983.447983.41402822PROCESSED57526.9620370375424754034.82883101853.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000011NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGGalactic bulgeNULLN
Eta Carinae161.281-59.6845287.6040589-0.62575348343.862153611.075034722253612.0627546296100012010497824000049790497824978249798222210055960.755960.785252.90PROCESSED57526.97730324075370553905.46488425933.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000012NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGEta CarinaeNULLN
N103B77.2315-68.7507279.61119012-34.3673096273.858653612.074016203753613.062627314810001301033064.64000033064.633064.633064.633064.6222210037281.437281.485405.91PROCESSED57526.97303240745424754034.87334490743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000013NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGN103BNULLN
E0102-7215.9813-72.0378301.56958331-45.05740554140.179853613.071064814853613.764050925910001401024333.92000024333.924333.924333.924333.9222210024514.424514.459863.92PROCESSED57511.51748842595370553905.46157407413.0.22.4313Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000014NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGXIS monitor with E0102-72NULLN
Crab Nebula83.637222.097184.48946706-5.7369784.999453613.832303240753613.9757870371000150105658.750005658.75658.75658.75658.711111005790.75790.712387.90PROCESSED57527.22964120375424754109.10532407413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000015NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD boresight check with CrabNULLN
Crab Nebula83.629622.1792184.41590928-5.6988995584.999853613.976215277853614.107731481510001502049505000495049504950495011111005117.85117.811359.90PROCESSED57527.22763888895424754109.10909722223.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000015NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD boresight check with CrabNULLN
Crab Nebula83.644922.0152184.56274906-5.7747315284.998753614.108344907453614.177175925910001503021005000210021002100210011111002307.42307.45943.90PROCESSED57527.2351504635424754109.39667824073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000015NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD boresight check with CrabNULLN
Crab Nebula83.644222.0129184.56435264-5.7765107784.997853614.83077546353614.90982638891000150402978.650002978.62978.62978.62978.611111003049.33049.36807.90PROCESSED57527.25024305565424754109.18156253.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000015NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD boresight check with CrabNULLN
Crab Nebula83.548422.0881184.45272098-5.8112169885.000453614.910300925953615.04185185181000150505344.750005344.75344.75344.75344.711111005485.95485.9113560PROCESSED57527.25113425935424754109.13579861113.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000015NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD boresight check with CrabNULLN
Crab Nebula83.72722.1071184.52563634-5.661279184.999653615.042465277853615.24321759261000150606525.650006525.66525.66525.66525.611111006759.96759.9173400PROCESSED57527.25344907415424754109.17153935183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000015NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD boresight check with CrabNULLN
Cas A350.825458.8156111.72292809-2.1247490112.993753614.248645833353614.76405092591000160102796520000279732797327973279652222100241302413044495.92PROCESSED57527.28321759265370553905.46596064823.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000016NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGCas ANULLN
Vega279.226438.769967.4321275319.23869014301.789653615.36734953753615.60358796310001701011398.51000011406.511406.511406.511398.5222210011575.111575.120403.90PROCESSED57527.26074074075424753906.07648148153.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000017NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGXIS OBF check with VegaNULLN
NEP272.788465.981495.7520272228.67554678290.929953615.613692129653617.625162037100018010106201.5100000106201.5106217.5106249.5106225.52222100106125106125173571.83PROCESSED57527.28800925935370553905.46369212963.0.22.436Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000018NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD background at North Ecliptic PoleNULLN
SN1006 NE BG226.7036-41.3998328.5140513514.65073262293.650353617.701886574153622.166828703710001901044750.35000044754.344754.344754.344750.3222210037388.337388.3385601.85PROCESSED57527.29231481485424754035.42247685183.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000019NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSN1006 observation with XIS and HXDNULLN
SN1006 NE-Rim225.9645-41.7797327.8225441414.6038019294.660653622.168321759353623.583553240710001902042844.25000042844.242852.642852.242848.2222210037615.637615.61221967PROCESSED57527.29236111115424754034.96468753.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000019NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSN1006 observation with XIS and HXDNULLN
SN1006 SW-Rim225.5051-42.0698327.3669254514.52303039297.271253623.586296296353624.99328703710001903028524.55000028532.528524.528540.928540.5222210027008.227008.2121551.95PROCESSED57527.31269675935424754034.96974537043.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000019NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSN1006 observation with XIS and HXDNULLN
SN1006 SW BG224.655-42.4005326.63273114.54333558310.488653624.999918981553626.007164351810001904032333.45000032333.432349.432341.432341.4222210024673.624673.687015.95PROCESSED57527.36474537045424754035.44826388893.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000019NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSN1006 observation with XIS and HXDNULLN
SN 1006 SW-Rim225.4961-42.0706327.3605224814.52564865117.271353761.091493055653761.715555555610001905028418.65000028418.628418.628418.628418.6222210024744.424744.4539100PROCESSED57532.78343755424754040.45866898153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000019NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSN1006 observation with XIS and HXDXISN
SN1006 SW BG224.6468-42.4025326.6262573914.54451897100.348953761.719965277853762.475277777810001906027981.35000027981.327989.327997.327997.3222210029550.429550.465249.92PROCESSED57532.79898148155424754040.56635416673.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000019NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSN1006 observation with XIS and HXDXISN
Fornax Cluster54.6395-35.4918236.7850293-53.61976834103.500253626.075601851853627.500266203710002001076078.210000076078.276078.276078.276078.2222210071112.871112.8123063.93PROCESSED57527.33774305565424754035.44420138893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000020NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGFornax ClusterNULLN
A0535+02684.724326.3189181.44092218-2.6442214683.60853627.569490740753628.0418865741100021010217612000021761217612176121761222210021257.221257.240783.91PROCESSED57527.31223379635424754035.06444444443.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000021We propose to observe the X-ray binary pulsar A0535+26. The main objectives is measuring changes in the cyclotron resonance energy in an outburst decay.It is known from another X-ray pulsar 4U0115+63 that the cyclotron resonance energy increased from 11 keV to 16 keV, as the luminosity decreased across a threshold luminosity of 4x10^37 erg/s. The flare of A0535+26 is a chance to know whether this behavior is the RULE among binary pulsars or an EXCEPTION. A0535+26 is fading down and will reach 30mCrab (5-100keV) on September 17, which is 5x10^36 erg/s. It is better to be observed as soon as possible, before it fades out.CALIBRATION1ASWGNULLNULLNULLJAP0SWGTOO Observation of A0535+026NULLN
Crab Nebula83.662221.1838185.27784655-6.2056513388.112553628.046805555653628.29881944441000220101288110000128811288112881128811111100122411224121767.90PROCESSED57527.3232754635424754109.25997685183.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000022Crab at 50arcmin off from the XIS aimpoint to study stray light.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab at 50 arcmin offNULLN
Crab Nebula82.732521.9883184.12771921-6.5022423988.097853628.300682870453628.583541666710002202010919.81000010919.810919.810919.810919.811111006340.16340.1244002PROCESSED57527.32626157415424754109.14863425933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000022Crab at 50arcmin off from the XIS aimpoint to study stray light.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab at 50 arcmin offNULLN
Crab Nebula84.528922.0469184.974122-5.0642479587.587953629.092175925953629.36827546310002203012824.41000012840.412832.412824.412848.4222210010351.810351.8238241PROCESSED57527.34780092595424754109.16215277783.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000022Crab at 50arcmin off from the XIS aimpoint to study stray light.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab at 50 arcmin offNULLN
Crab Nebula83.628222.0761184.5027205-5.7552036387.7953628.585219907453628.826539351810002301011997.81000011997.811997.811997.811997.8111110010513.210513.220823.90PROCESSED57527.33559027785424754109.22682870373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000023Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab at nominal positionsNULLN
Crab Nebula83.630922.0151184.55585082-5.7857481687.846653628.826921296353629.090497685210002302012527.11000012531.112527.112536.412535.1222210013352.913352.9227641PROCESSED57527.34091435185424754109.1935995373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000023Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCrab at nominal positionsNULLN
NGC 211088.0444-7.458212.92660512-16.54877043103.418853629.379629629653631.8308333333100024010101748.7100000101926.5103760.1101748.7102148.3222210086043.386043.3211755.84PROCESSED57527.40303240745424754035.46241898153.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000024The Narrow Emission Line Galaxy NGC 2110 was the brightest AGN in the initial BAT survey release (BAT flux of 2.1E-10 erg/cm2/sec) visible to Suzaku during Sept./Oct., and is still currently bright in BAT. A 2003 RXTE observation yielded F_2-10 keV = 4E-11 erg/cm2/sec. The source is currently almost 3 times brighter than during the SAX observations. The main goals are to measure the high energy cutoff and to place a strong limit on the presence of reflection. The Compton reflection hump is weak in SAX data (suggesting that the Fe K line originates in Compton-thin material). Determining the strength of the reflection component is critical for constraining the geometry of the accreting material.CALIBRATION1ASWGNULLNULLNULLJAP0SWGNarrow Emission Line Galaxy NGC 2110NULLN
BD +30 3639293.688730.505164.775568775.01383279277.871353634.381493055653635.247384259310002501035214.64000035230.635230.635214.635222.6222210033372.833372.874803.91PROCESSED57527.39315972225424754035.46645833333.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000025The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time.CALIBRATION1ASWGNULLNULLNULLJAP0SWGObservation of planetary nebula BD +30 3639NULLN
BD +30 3639293.699330.506564.781198995.00649051237.734253676.993483796353677.823032407410002502031138.44000031138.431162.431146.431154.4222210027125.827125.8716381PROCESSED57527.93155092595424754037.10809027783.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000025The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time.CALIBRATION1ASWGNULLNULLNULLJAP0SWGObservation of planetary nebula BD +30 3639NULLN
RXJ1713.7-3946258.074-39.935347.05133682-0.37925502269.997753639.656319444453641.296064814810002601068495.98000068495.968565.368511.968525.3222210056238.256238.2141661.90PROCESSED57527.45619212965424754037.07506944453.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000026RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons.CALIBRATION1ASWGNULLNULLNULLJAP0SWGObservation of RXJ1713.7-3946NULLN
RXJ1713-3946-BKGD1257.3853-38.8228347.632239850.70836337270.009153638.799768518553639.654270833310002602034928.44000034928.434928.434928.434928.4222210028371.328371.373819.90PROCESSED57527.4323495375424754035.53474537043.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000026RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons.CALIBRATION1ASWGNULLNULLNULLJAP0SWGObservation of RXJ1713.7-3946NULLN
RXJ1713-3946-BKGD2257.2742-41.0338345.80577047-0.54060643270.003353641.298067129653642.184305555610002603037513.24000037537.237529.237513.237513.2222210031898.231898.276565.90PROCESSED57527.44615740745424754035.61872685183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000026RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons.CALIBRATION1ASWGNULLNULLNULLJAP0SWGObservation of RXJ1713.7-3946NULLN
Sgr_A_East266.5146-28.92670.05802898-0.07696746264.715253636.304456018553637.46202546310002701044785500004480144852.34478544828.3222210037854.337854.3100013.91PROCESSED57527.41886574075424754035.5026620373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000027We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.CALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Observation of Galactic Center RegionNULLN
Sgr_A_west266.3057-29.1697359.75546849-0.04768885264.960153637.595335648253638.727303240710002702042814.85000042814.842814.842814.842814.822221003609136091978000PROCESSED57527.42938657415424754035.51355324073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000027We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.CALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Observation of Galactic Center RegionNULLN
1A1742-294(GC_BGD_1)266.5264-29.516359.56008755-0.392308264.866453637.46328703753637.5279629631000270302066.350002066.32066.32066.32066.311111001887.71887.755840PROCESSED57527.40004629635424754035.46395833333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000027We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.CALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Observation of Galactic Center RegionNULLN
KS1741-293(GC_BGD_2)266.2069-29.3515359.55541243-0.06909433265.017453637.528854166753637.594629629610002704019375000193719371937193711111001763.71763.756800PROCESSED57527.4045254635424753907.3932754633.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000027We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.CALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Observation of Galactic Center RegionNULLN
1E1743.1-2843(GC_BGD_3)266.592-28.65160.328287050.00813221264.8853638.728611111153638.7932754631000270501984.650001984.61984.61984.61984.611111001793.41793.45567.90PROCESSED57527.40930555565424753905.63430555563.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000027We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.CALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Observation of Galactic Center RegionNULLN
HESS J1616-508244.1248-50.8971332.40352084-0.15000913282.847653632.500023148253633.8183333333100028010413525000041352413764135241368222210035373.135373.1113889.90PROCESSED57527.38381944445424754035.43611111113.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000028NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGNew HESS sources and the Galactic ridge BackgroundNULLN
HESS J1616-508_BGD1243.666-51.1742332.00349288-0.15039556283.006253631.949722222253632.499085648210002802019327.72500019327.7206301936019632.3111110016642.616642.647447.90PROCESSED57527.35731481485424754035.16924768523.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000028NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGNew HESS sources and the Galactic ridge BackgroundNULLN
HESS J1616-508_BGD2244.4656-50.6883332.70353325-0.14997577283.179353633.819641203753634.312083333310002803021873.52500021889.521889.521881.521873.5111110018206.318206.342535.90PROCESSED57527.37228009265424754035.46988425933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000028NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGNew HESS sources and the Galactic ridge BackgroundNULLN
GRO J1655-40253.5027-39.8455344.983159762.45489032268.023753635.314062553636.296805555610002901035222.840000035233.635222.835230.8012210028731.528731.584901.91PROCESSED57527.39973379635424754035.49406253.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000029We propose to observe GRO J1655-40, a transient galactic black hole candidate. With M=~7 Msolar and distinct radio lobes, GRO J1655-40 has been classified as a microquasar. It was highly variable during the first few years after its discovery while showing irregular flaring and a wide range of continuum states. Discrete Fe K absorption structure was observed with ASCA. In the summer of 1997 it entered an extended quiescence that lasted for ~8 years. In March 2005 it became active again and XMM & Chandra have observed it since. Only Suzaku can provide the broadband sensitivity required to map the Fe K structure and the continuum as they change. GRO J1655-40 is rapidly declining and must be observed soon before it reenters quiescence.CALIBRATION1ASWGNULLNULLNULLJAP0SWGGRO J1655-40NULLN
A 2218249.000166.20397.72440138.11892096242.361753644.364340277853645.344664351810003001043362.95000043362.944717.343425.343824.8222210041491.841491.8846781PROCESSED57527.47918981485424754035.76773148153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000030Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far.CALIBRATION1ASWGNULLNULLNULLJAP0SWGA2218 and its offset observationNULLN
A2218_offset244.476965.446897.7205947540.11912915237.196553645.347453703753646.3237510003002044859.25000044859.246190.744914.145374.7222210042536.642536.684343.90PROCESSED57527.52031255424754036.9692245373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000030Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far.CALIBRATION1ASWGNULLNULLNULLJAP0SWGA2218 and its offset observationNULLN
NGC3516166.729972.5779133.217965242.40001774148.936653655.581354166753658.3801388889100031010134469.6150000134509.6134595.6134509.6134469.62222100122818122818241684.80PROCESSED57527.62436342595424754036.47049768523.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000031NGC 3516 is one of the brightest Seyfert 1s seen in BAT currently visible to Suzaku. Recent BAT and RXTE observations show that this source is ~2-3 mCrb in the 2-10 keV band and ~4-5 mCrb in 15-100 keV. NGC 3516 is currently much brighter than when XMM observed it in 2000 (e.g., it has since returned to "typical" flux). This source's Fe K line and Compton reflection hump are both quite strong (e.g., as seen with SAX; R is ~1.8 in SAX data).CALIBRATION1ASWGNULLNULLNULLJAP0SWGNGC 3516NULLN
ULXs in NGC 131349.5245-66.5352283.41323765-44.63106544172.633753658.55640046353659.62527777781000320103287840000328783287832878328781111100303803038092343.91PROCESSED57527.5873495375424754036.19293981483.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000032We propose Suzaku observation of a nearby (4.5 Mpc) galaxy NGC 1313 hosting two prototypical ULXs. These ASCA specta of many ULXs were described with a "high temperature diskbb" model, spectra obtained with XMM (and Chandra) prefer a "power-law plus low-temperature disk" modeling. The superior 5-10 keV sensitivity of Suzaku allows us to examine whether the spectra of luminous ULXs indeed exhibit a turn-over around 5 keV or extend up to 10 keV.CALIBRATION1ASWGNULLNULLNULLJAP0SWGULXs in NGC 1313NULLN
M82-Wind148.889369.7655141.3388028440.49464345137.760853647.507280092653648.141828703710003301032327.410000032327.432327.432327.432327.4222210030222.430222.454802.10PROCESSED57527.51550925935424754037.00571759263.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000033We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec.CALIBRATION1ASWGNULLNULLNULLJAP0SWGLargely Extended Emission (~12kpc) around M82NULLN
M82-Wind148.89469.7643141.3388388440.49666381146.24653662.040127314853662.939039351810003302040358.610000040358.640382.640358.640366.6222210038353.338353.3776580PROCESSED57527.61275462965424754036.41962962963.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000033We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec.CALIBRATION1ASWGNULLNULLNULLJAP0SWGLargely Extended Emission (~12kpc) around M82NULLN
M82-Wind148.888569.7652141.3393354740.4945935137.760853670.468113425953671.100219907410003303028363.810000028379.828379.828371.828363.8222210025812.125812.1546041PROCESSED57527.67846064825424754036.86394675933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000033We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec.CALIBRATION1ASWGNULLNULLNULLJAP0SWGLargely Extended Emission (~12kpc) around M82NULLN
A 337690.5561-39.9584246.50686261-25.98989573107.612453649.615370370453653.4495833333100034010118779.2150000118779.2121737.3118849.8119335.72222100100540.1100540.1331253.73PROCESSED57527.62181712965424754109.63969907413.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000034Abell 3376 (z=0.046) is a merging cluster with a T=4 keV (*3) hosting a pair of strong radio halos (see figure). It is one of the few clusters from which BeppoSAX positively detected excess hard X-rays (Nevalainen et al. ApJ 608, 166, 2004). Because of the relatively low temperature, the HXD-PIN energy band is expected to be relatively free from thermal emission, making this object ideal to the search for non-thermal signals. We expect the non-thermal flux to be 4-5% of the PIN background at 20 keV, and a 150 ksec on-source exposure would be needed to securely detect this. To know the current background over the full COR range, an off-source exposure for one day or a ~40 ksec exposure onto a very soft source, would be required immediately before or after the on-source data acquisition.CALIBRATION1ASWGNULLNULLNULLJAP0SWGDiffuse Hard X-rays from ClustersNULLN
Her X-1254.46535.330658.1356243837.51514805249.571453648.645046296353649.434189814810003501036123.54000036923.536123.536923.536923.5212210033322.933322.9681780PROCESSED57527.55935185185424754036.00843753.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000035NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGHXD Performance Verification using Her X-1NULLN
CYG X-1299.590735.189271.324549043.06010347276.989853648.202534722253648.6335532407100036010182132000018213182131821318213111110018145.718145.737229.90PROCESSED57527.55987268525424754037.72788194443.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000036We propose to probe the geometry of optically-thick accretion disks which should exist around a BH even in the hard state and to verify the HXD performance to thermal cut-off in hard X-rays expected from AGN. The 1st may be done by measuring the cool disk emission with the XIS-BI, resolving the fluorescent Fe-K line with the XIS-FI and detecting the reflection continuum with the HXD. Since these features are thought to come from the optically-thick disk a simultaneous measurement will for the 1st time allow for self-consistent constraining of the disk geometry in the hard state. Cyg X-1 is the best & most secure object for this stufy and is now in the low/hard state. A 20 ks Suzaku obs. is sufficient to get a fine spectrum up to 300 keV & to determine the cutoff with a high significance.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCyg X-1 in the low stateNULLN
Sgr_A_west266.3063-29.1685359.75676556-0.04750971264.960453642.191446759353643.18702546310003701043741.25000043741.243749.243749.243749.2222210039394.139394.186013.90PROCESSED57527.45818287045424754035.66633101853.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
1A1742-294(GCBGD1)266.5239-29.5135359.5610912-0.38914955264.867353643.188009259353643.253692129610003702032735000328132733288.7328111111003091.13091.15671.90PROCESSED57527.44253472225424754035.55474537043.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
KS1741-293(GCBGD2)266.2067-29.3539359.55327497-0.0701996265.016253643.25453703753643.320370370410003703029705000299429862978297022221002824.42824.45679.90PROCESSED57527.44804398155424754035.77741898153.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
Sgr_A_East266.5133-28.92660.05752244-0.07594372264.715953643.321539351853644.264861111110003704042917.65000042957.642961.642917.642939.2222210039453.339453.3814941PROCESSED57527.47533564825424754035.76196759263.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
1E1743.1-2843 GCBGD3266.5944-28.65260.328527190.00581314264.879853644.265752314853644.316226851810003705024005000240024002400240022221002232.92232.94353.90PROCESSED57527.45309027785424754056.19708333333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
Sgr_B2266.8775-28.44350.63628385-0.09835114265.372753653.519456018553655.295405092610003706076596.610000076628.676644.676596.676628.6222210070819.270819.2153431.90PROCESSED57527.57760416675424754036.22627314823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
Sgr_B2_BGD267.0943-28.13560.99854005-0.10262599269.020853655.298888888953655.46208333331000370709161.2100009161.29164.39164.39163.222221009536.49536.4140920PROCESSED57527.56880787045424754036.07498842593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000037NULLCALIBRATION1ASWGNULLNULLNULLJAP0SWGSuzaku Obseration of Galactic Center region 2NULLN
NORTH POLAR SPUR260.59054.748926.8341219721.95376599264.114353646.478576388953647.451527777810003801043068.95000043148.944212.943068.943292.9222210040771.540771.584001.90PROCESSED57527.53428240745424754035.89280092593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000038We propose to observe the North Polar Spur for 100 ksec. The main objectives are below (1) Search for emission lines of N and C that originates from low kT emission (2) Precisely determine the abundance of the NPS The measurement of N and C lines will be the first for XIS. This is also the first for extended sources. The first trial to measure the emission from the C-band (below 0.3keV) by using BI. This will be a guide line how to use the C-band data. Since the C-band intensity is already known, this will be the first calibration of the BI at low energy. The scientific objectives are already given in the mail distributed in the swg.CALIBRATION1ASWGNULLNULLNULLJAP0SWGNorth Polar SpurNULLN
GRS1915+105288.801410.936845.35928754-0.22611181260.576253659.695196759353661.972430555610003901084777.78000085063.186430.585071.184777.7333310068862.368862.3196733.82PROCESSED57527.91885416675424754043.81174768523.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000039This observation will be performed as a part of the big multiwavelength campain including Suzaku, VLA, Integral, RXTE, and Spitzer.CALIBRATION1ASWGNULLNULLNULLJAP0SWGCampaign of coordinated observation of GRS 1915+105NULLN
MKN 393.883971.0477143.283630122.7163146371.832653665.084826388953667.268217592610004001095026.510000095026.595077.295045.295034.5222210091344.191344.1188629.90PROCESSED57527.66430555565424753906.48967592593.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000040Mkn 3 is the second brightest Compton-thick Sy 2 currently visible with Suzaku. The broadband spectrum of Mkn 3, as probed by previous SAX and Chandra observations, is dominated by a reflection component (Compton hump strength R is near 1), but there is also evidence for a strongly absorbed hard X-ray power law that may be direct emission from the obscured nucleus, filtering through Compton-thick material (such as the molecular torus).CALIBRATION1ASWGNULLNULLNULLJAP0SWGMKN 3HXDN
RXJ1856.5-3754284.1498-37.9103358.59888263-17.21635309269.425953667.282997685253669.479328703710004101076254.880000076254.800020010062621.762621.71897203PROCESSED57527.68111111115424754037.22947916673.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000041We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them.CALIBRATION1ASWGNULLNULLNULLJAP0SWGLOW ENERGY QE CALIBRATION OF XISXISN
RXJ1856.5-3754284.1433-37.91358.59722216-17.2114669784.012753817.938807870453819.4433217593100041020791698000079177791697917779177222210053209.953209.9129975.91PROCESSED57533.33252314825424754042.29678240743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22000041We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them.CALIBRATION1ASWGNULLNULLNULLJAP0SWGLOW ENERGY QE CALIBRATION OF XISXISN
CAS A350.872958.8094111.74406014-2.13880346214.737253768.536365740753768.8335995371000430100100000000000010010326.810326.825673.91PROCESSED57532.84517361115424754040.74888888893.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001097We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chipCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP0SWGXIS FLIGHT CAIBRATION PLANXISN
CAS A350.876158.8091111.74552355-2.13963884214.553753783.600347222253783.9218055556100043020141551000014155141551415514155111110017371.317371.3277680PROCESSED57533.03118055565424754041.46278935183.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001097We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chipCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP0SWGXIS FLIGHT CAIBRATION PLANXISN
E0102-7215.9926-72.0236301.56327722-45.07133229226.832653720.071620370453723.4377199074100044010597312000059735125919.559731597373333100115330.2115330.2290803.71PROCESSED57532.58039351855424754119.76126157413.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001097We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chipCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP0SWGXIS FLIGHT CAIBRATION PLANNULLN
E0102-7216.0206-72.0231301.55102123-45.07123322281.39653752.974270833353755.375219907410004402041260.5200004126841852.441260.541361343410099793.599793.5207429.83PROCESSED57532.75555555565424754040.69795138893.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001097We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chipCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP0SWGXIS FLIGHT CAIBRATION PLANXISN
E0102-7216.027-72.0223301.54815221-45.07189388294.075153768.846759259353769.406539351810004403020827.72000020835.720843.720843.720827.7222210020268.820268.8483601PROCESSED57532.86157407415424753905.67643518523.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001097We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chipCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP0SWGXIS FLIGHT CAIBRATION PLANXISN
ETA CARINAE161.248-59.6859287.58997588-0.63475906156.12453769.416319444453769.948194444410004501021367.82000021367.821367.821367.821367.8222210018145.818145.845945.91PROCESSED57532.93699074075424754040.98466435183.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001097We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chipCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP0SWGXIS FLIGHT CAIBRATION PLANXISN
LOCKMANHOLE163.406357.6108148.9819317953.14624927119.61153688.237233796353689.830069444410004601076980.610000076980.677044.677012.677020.6222210094510.794510.7137607.93PROCESSED57528.00481481485424754037.58898148153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001098We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background.CALIBRATION1AKOKUBUNMOTOHIDENULLNULLJAP0SWGBACKGROUND ESTABLISHMENT OF HXDXISN
GALACTIC CENTER266.5135-28.92690.05735731-0.07624929270.249553986.099583333353987.379340277810004801063007.95000063007.963007.963007.963007.9222210060322.860322.8110567.92PROCESSED57535.52019675935452654056.48491898153.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1SWGXIS FLIGHT CALIBRATION PLANXISN
CYGNUS LOOP314.034531.931175.67403832-8.6167654164.226153884.155601851853884.37938657411000490108380.5100008380.58380.58380.58380.511111006021.16021.1193040PROCESSED57534.46282407415425854059.4110995373.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1SWGXIS FLIGHT CALIBRATION PLANSPEN
CYGNUS LOOP314.078532.043875.78588033-8.5735824364.226353884.379675925953884.60863425931000490207892.8100007892.87892.87892.87892.822221007452745219769.90PROCESSED57534.46748842595425854088.84295138893.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1SWGXIS FLIGHT CALIBRATION PLANSPEN
CYGNUS LOOP313.949432.081875.74490282-8.4650845364.229253884.608923611153884.837777777810004903011697.11000011705.111697.111705.111705.1222210012268.812268.8197720PROCESSED57534.47228009265425854052.49150462963.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1SWGXIS FLIGHT CALIBRATION PLANSPEN
CYGNUS LOOP313.903731.969675.63250703-8.5067052664.224553884.838067129653885.089166666710004904011765.61000011781.611781.611773.611765.611111009788978821687.90PROCESSED57534.47712962965425854052.52011574073.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1SWGXIS FLIGHT CALIBRATION PLANSPEN
HER X-1254.422435.408358.2253566437.5618523267.878353823.766990740753824.64046296310100101033062.14000033062.138804.533062.133070.1434410026222.826222.875437.90PROCESSED57526.81787037045382653906.98759259263.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015002The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO.CALIBRATION1AKOKUBUNMOTOHIDENULLNULLJAP1AO1SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATIONHXDN
LOCKMAN HOLE162.936657.2557149.7034431453.20093146281.872153872.738958333353874.793958333310100201080398.28000080398.280406.280406.280406.233331008885488854177513.84PROCESSED57534.36942129635382653927.76898148153.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015003We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD.CALIBRATION1AKOKUBUNMOTOHIDENULLNULLJAP1AO1SUZAKU OBSERVATION OF LOCKMANHOLEXISN
CRAB83.656921.9577184.61755594-5.79610428250.942453830.546342592653831.592511574110100301037832.34000037832.337853.337832.337832.31111100309893098990379.91PROCESSED57533.43237268525382653907.13069444453.0.22.436Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015004Crab cal at the XIS and HXD nominal positions.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRABHXDN
CRAB83.637122.0108184.56259415-5.78319491253.331853824.65265046353825.166886574110100401016363.22000016363.216372.8163651636511111009761.69761.6444260PROCESSED57533.33780092595382653906.06218753.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015004Crab cal at the XIS and HXD nominal positions.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRABXISN
CRAB83.636822.0131184.56049184-5.78219867250.94353829.129664351853829.597430555610100402019138.92000019138.919145.819138.919138.9111110013283.113283.140411.91PROCESSED57533.37780092595382653906.64093753.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015004Crab cal at the XIS and HXD nominal positions.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRABXISN
E0102.2-721916.0331-72.0338301.54662861-45.060290668.202453841.40421296353841.9793865741101005010213244000021340213242133221340111110016683.116683.149663.90PROCESSED57533.46512731485382653905.69384259263.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721916.0278-72.0394301.54948943-45.054818234.413653876.71952546353877.179328703710100502018161.92000018161.918193.918161.918193.9212110017763.317763.339719.90PROCESSED57534.38384259265382653926.14222222223.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721916.0175-72.0405301.55408267-45.0539416560.635353912.866273148253913.424583333310100503021675.82000021715.821683.821715.821675.8242410035062.635062.648203.90PROCESSED57534.75848379635382653928.45864583333.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721915.9978-72.0424301.56284618-45.0524664492.979453933.265659722253933.903043981510100504022063.42000022063.422103.422063.422095.4424210020982.320982.355047.91PROCESSED57534.96138888895382653942.46300925933.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721915.9824-72.0369301.56901677-45.05828014133.823253972.205266203753973.393333333310100505068363.22000068987.268363.268987.268971.2555610068002.468002.4102633.91PROCESSED57535.36184027785382654020.99290509263.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721915.9812-72.0315301.5690149-45.06369281159.245353997.226342592653997.56266203710100506010790.74000010806.710806.710790.710798.7222210010322.310322.3290500PROCESSED57535.62635416675382654021.13251157413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721915.9801-72.0277301.56912514-45.06750714192.885554029.65062554030.226562510100507037130.54000037170.537130.537170.537162.5333310036471.636471.6497600PROCESSED57535.90634259265382654055.56318287043.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0029-72.0223301.55865958-45.07240987252.270954082.786990740754083.127997685210100509028226200002822628226028226110110023054.623054.629455.90PROCESSED57536.32581018525382654094.59303240743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0137-72.0201301.5537348-45.07437383265.990554115.139502314854115.665555555610100510022614200002261422614022614110110019149.619149.6454241PROCESSED57536.83232638895382654132.85094907413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721916.0273-72.0256301.54834682-45.06859544302.813154141.926238425954142.81266203710100511036093.82000036101.836093.8036101.8110110052703.852703.876575.91PROCESSED57537.35675925935382654153.22274305563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0373-72.0314301.54456169-45.06259438341.000654177.882858796354178.299467592610100512018242200001824218250018258110110014755.114755.135983.90PROCESSED57537.69706018525382654185.44590277783.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
PKS2155-304329.7138-30.225917.72949775-52.2431888857.901353856.260092592653857.250104166710100601038551.53000038551.538551.538551.538551.5222210023947.623947.685514.12PROCESSED57533.60807870375382653913.27738425933.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
RXJ1856.5-3754284.1489-37.9077358.6011477-17.21474589254.295354028.512847222254029.640520833310100901040784.14000040784.140784.140784.140784.1222210035169.935169.997403.91PROCESSED57535.92196759265382654055.47325231483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015007Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS FLIGHT CALIBRATION PLANXISN
CRAB83.630122.0172184.55366892-5.7852503885.702653983.222743055653983.819664351810101001020717.52000020877.520717.520893.520885.5323310019607.119607.151569.91PROCESSED57535.4642245375382654024.66958333333.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015014HXD cal.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP1AO1CRAB CAL FOR HXD ON 2006 AUTUMNXISN
THE CRAB OFFSETS83.620922.1323184.45137768-5.7308213585.713253983.819953703753983.88910879631010110103348200033483348334833481111100367636765967.90PROCESSED57535.45482638895382654104.44182870373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.622922.105184.47554642-5.7438763385.714653983.88921296353983.95160879631010110203350200033503350335033501111100300430045383.90PROCESSED57535.46006944445382654104.43741898153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.625422.076184.50140903-5.7574486185.716453983.95171296353984.090497685210101103067032000670367036703670311111005445.85445.811983.90PROCESSED57535.46504629635382654104.9726504633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSHXDN
THE CRAB OFFSETS83.627422.0499184.52456216-5.7698576785.71953984.090601851853984.15299768521010110403353200033533353335333531111100241424145383.90PROCESSED57535.46619212965382654104.41435185183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.632321.9916184.57650041-5.7972316885.724453984.153194444553984.22244212961010110503355200033553355335533551111100218721875975.90PROCESSED57535.47449074075382654104.44785879633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.633121.9589184.60466298-5.8141084487.506253996.875868055653996.95155092591010110603368200033683368336833681111100271627166527.90PROCESSED57535.61138888895382654104.42314814823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.633821.931184.62870178-5.8284928987.510353996.951655092653997.01405092591010110702636200026362636263626361111100215721575383.90PROCESSED57535.61300925935382654104.41600694443.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.634321.9041184.65179297-5.8424976887.509453997.014155092653997.08349537041010110802251200022512251225122511111100227522755983.91PROCESSED57535.61824074075382654104.44696759263.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.755522.0251184.60946275-5.6828055487.896353997.084062553997.152928240710101109018952000189518951895189522221002081.52081.55945.90PROCESSED57535.61914351855382654104.45177083333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.724122.023184.59560566-5.7085270387.548453997.153449074153997.215451388910101110015452000154515451545154511111001806180653560PROCESSED57535.6195370375382654104.43377314823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.692722.0229184.58004352-5.733175885.75653984.568009259353984.62521990741010111102635.420002635.42635.42635.42635.411111002457.32457.349420PROCESSED57535.47150462965382654104.43215277783.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.661622.0194184.56751127-5.7594055685.747353984.625370370453984.68769675931010111202976.120002976.12976.12976.12976.122221002802280253800PROCESSED57535.47384259265382654104.42545138893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.599122.0137184.54117278-5.8113971485.724953984.687939814853984.75722222221010111303366.120003366.13366.13366.13366.11111100319031905983.90PROCESSED57535.47704861115382654104.45753.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.567522.0116184.5271819-5.837261485.713153984.757326388953984.81972222221010111403369200033693369336933691111100363236325383.90PROCESSED57535.48025462965382654104.42706018523.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.53622.0119184.51119717-5.861758385.70353984.819826388953984.889166666710101115033702000337033703370337011111003347.23347.25983.90PROCESSED57535.48241898155382654104.97304398153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
THE CRAB OFFSETS83.505622.0085184.49889553-5.8873741885.693953984.889270833353984.9351010111602765.120002765.12765.12765.12765.11111100215221523943.90PROCESSED57535.48270833335382654104.45084490743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015015We propose observing multiple offset pointings of the Crab nebula.CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP1AO1CRAB OFFSET POINTINGSSPEN
PERSEUS CLUSTER49.943641.5175150.56798595-13.2592938766.039353976.78827546353980.0793865741101012010150905.1150000150905.1150921.1150937.1150921.16666100142533.4142533.42843363PROCESSED57535.51593755382654024.86487268523.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015016We propose the observation of Perseus cluster for 150ks. To recover the energy resolution of the XIS, we will try the periodic charge injection method. However, the charge injection will change calibrations such as gain, QE and so on dramatically. To study the change of the clibrations, Perseus cluster is one of the best targets, because it is extended over the whole XIS FOV and the iron K line from the cluster is extremely strong. For the first 50ks, the observation will be done with the normal mode without the charge injection. For the second and third 50ks, we will do the charge injections with every 54 and 108 rows, repectively.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1PERSEUS OBSERVATION FOR CALIBRATIONS ON THE PERIODIC CHARGE INJECTION METHODXISY
PERSEUS CLUSTER49.954241.5047150.58204074-13.26559499258.651554136.665138888954137.604328703710101202043871.44000043895.443879.4043871.4220210041573.241573.281137.91PROCESSED57537.33569444445382654151.65423611113.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015017we propose observations for the XIS flight calibrations during the left term of AO-1.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS CALIBRATIONS FOR AO1XISY
CYGNUS LOOP314.011831.991275.70842949-8.56360013217.464254090.395393518554090.6848842593101013010910210000910291020910222021009212.69212.6250061PROCESSED57536.3732754635382654108.45719907413.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015017we propose observations for the XIS flight calibrations during the left term of AO-1.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS CALIBRATIONS FOR AO1XISY
CYGNUS LOOP314.013331.99275.70987313-8.56406979213.211754090.686979166754091.117523148210101302021004200002100421004021004110110018871.918871.9371681PROCESSED57536.38851851855382654132.70857638893.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015017we propose observations for the XIS flight calibrations during the left term of AO-1.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS CALIBRATIONS FOR AO1XISY
CYGNUS LOOP314.012931.992575.71004378-8.56348961212.846854091.118043981554091.603634259310101303019729.52000019729.519729.5019729.5220210020100.520100.541927.91PROCESSED57536.39311342595382654132.73756944443.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22015017we propose observations for the XIS flight calibrations during the left term of AO-1.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP1AO1XIS CALIBRATIONS FOR AO1XISY
E0102.2-721916.0421-72.0341301.54273778-45.059797482.539154200.441064814854200.8127199074102001010181152000018115181150181151101100245232452332103.90PROCESSED57538.10623842595419154210.60372685183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0153-72.0406301.55505042-45.0538889560.669354264.4237554265.146747685210200201027871.72000027871.727871.7027871.7220210028315.528315.562463.91PROCESSED57538.93737268525419154271.45050925933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721915.9919-72.0394301.56512259-45.05558467110.195654324.223020833354325.156527777810200301039482200003949039482039490110110037350.537350.580647.91PROCESSED57539.48106481485419154347.47957175933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721915.9812-72.0282301.56869429-45.06698503193.181254398.517187554399.37516203710200401026175.72000026175.726175.7026175.7220210025480.725480.774093.80PROCESSED57540.36100694445419154407.52604166673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0039-72.0219301.55818443-45.07278758249.458254435.809490740754436.409942129610200501024766.72000024766.724790.7024790.7110110023722.323722.351871.91PROCESSED57540.76758101855419154441.01084490743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0383-72.0304301.54402708-45.06357038338.154540.238506944454540.864861111110200601028238.92000028238.928238.9028238.9220210038612.638612.6541140PROCESSED57541.87107638895419154550.22503472223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP313.988432.00475.70560343-8.5401512944.001654263.552083333354263.866840277810200701013345.51000013353.513345.5013353.5220210012560.712560.727191.91PROCESSED57538.90701388895419154269.41170138893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP314.007231.986275.70201861-8.56378367248.018654437.21922453754437.562731481510200801013265.51000013265.513265.5013265.5220210013271.613271.6296760PROCESSED57540.78277777785419154445.18627314823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP313.988232.003575.70510458-8.5403394343.758954263.867314814854264.41202546310200901022896.52000022896.522900.5022916.5330310018570.818570.8470600PROCESSED57538.91628472225419154269.42754629633.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
CYGNUS_LOOP_55FE314.006531.986275.70163572-8.56332634247.751954437.563159722254438.189074074110201001029585200002958529585029585330310027780.427780.454075.90PROCESSED57540.79122685185419154451.46479166673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
PERSEUS CLUSTER49.946141.5179150.56936377-13.2579280883.37654327.528344907454328.47733796310201101042281.74000042281.742281.7042281.7220210036206.336206.381983.91PROCESSED57539.62150462965419154347.60708333333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
PERSEUS_CLUSTER_Normal49.956541.505150.58334697-13.26439478255.186154503.090069444454504.437719907410201201061742.64000061742.661742.6061742.6440410062315.762315.7116399.90PROCESSED57541.54928240745419154515.83017361113.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
GALACTIC CENTER266.5129-28.92780.05631549-0.07626904265.297254346.792476851854348.222453703710201301051396500005139651420051404220210044477.844477.8123535.80PROCESSED57539.94401620375419154356.39513888893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
RXJ1856.5-3754284.1483-37.9083358.60038232-17.21452318271.934554388.728993055654389.58702546310201401041318400004131841318041318220210040654.540654.574129.91PROCESSED57540.29185185185419154403.0604629633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
RXJ1856.5-3754284.1438-37.9098358.59756743-17.2117616789.704154547.269340277854548.472384259310201501050652.34000050652.350668.3050652.3220210038365.438365.4103923.82PROCESSED57541.9456255419154566.31575231483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISY
PSR 1509-58 AT NOM.228.4878-59.1337320.32453924-1.16169081289.211954333.563206018554334.104444444410201601041213.84000041221.841221.8041213.8110110032908.432908.446759.91PROCESSED57539.64343755419154350.41468753.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025156PSR 1509-58CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP2AO2PSR 1509-58XISY
PSR 1509-58 AT FIXEA228.4815-59.094320.34236207-1.12606748287.632954334.105706018554334.769027777810201701043803.84000043843.843827.8043803.8220210037119.937119.957303.93PROCESSED57539.64531255419154350.66584490743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025156PSR 1509-58CALIBRATION1AMAEDAYOSHITOMONULLNULLJAP2AO2PSR 1509-58XISY
LOCKMANHOLE162.925757.2581149.7070797453.19495056319.51254223.966759259354226.083553240710201801096071.68000096079.696079.6096071.622021009277892778182824.83PROCESSED57538.61012731485419154230.45559027783.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025157The purpose of this observation is to verify the energy response of HXD-PIN/GSO.CALIBRATION1AKOKUBUNMOTOHIDENULLNULLJAP2AO2CALIBRATION OBSERVATION OF HXD WITH CRABXISY
CRAB83.635721.9546184.60961134-5.81437304269.389854179.445740740754180.600891203710201901047633.14000047633.147633.1047633.1320310043407.543407.599773.91PROCESSED57537.81239583335419154314.66315972223.0.22.436Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025158The purpose of this observation is to verify the energy response of HXD-PIN/GSO.CALIBRATION1AKOKUBUNMOTOHIDENULLNULLJAP2AO2CALIBRATION OBSERVATION OF HXD WITH CRABHXDY
PKS2155-304329.716-30.226817.72837689-52.2451769458.205854212.520879629654212.848831018510202001012036.61500012036.612036.6012036.61101100105721057228327.91PROCESSED57538.44612268525419154217.22575231483.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025160This is a coordinated observation of PKS2155-304 with Chandra and XMM-Newton for spectral calibration. The observation also aims at evaluating the amount of contaminant on the XIS OBF.CALIBRATION1AISHIDAMANABUNULLNULLJAP2AO2PKS2155-304 COORDINATED WITH CHANDRA AND XMM-NEWTONXISY
E0102.2-721915.976-72.0294301.57107704-45.06589786179.782854371.259583333354371.639050925910202101025314.61200025314.625314.6025314.62202100202252022532781.90PROCESSED57540.12923611115419154402.27494212963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025155The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP2AO2XIS FLIGHT CALIBRATION PLANXISN
E0102.2-721916.0349-72.0243301.54490568-45.06972875306.723754510.706574074154512.132222222210202201048424.54000048424.548437.3048432.5320310046842.146842.1123151.80PROCESSED57526.88769675935419154553.21325231483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220251614 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode.CALIBRATION1ASWGNULLNULLNULLJAP2AO2SUZAKU ADDITIONAL CALIBRATIONXISY
PSR B0540-6985.0333-69.3191279.70305196-31.5216772241.330354512.137233796354513.44453703710202301052168.94000052168.952168.9052168.922021004645946459112937.81PROCESSED57541.58917824075419154522.22832175933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220251614 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode.CALIBRATION1ASWGNULLNULLNULLJAP2AO2SUZAKU ADDITIONAL CALIBRATIONXISY
HER X-1254.458935.355758.1658562837.52408174104.616854517.627673611154518.486388888910202401038931400003893938931038939220210034312.134312.1741902PROCESSED57541.70365740745419154525.48951388893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220251614 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode.CALIBRATION1ASWGNULLNULLNULLJAP2AO2SUZAKU ADDITIONAL CALIBRATIONXISY
E0102.2-721916.0298-72.0236301.54705976-45.07053683295.981754501.057199074154501.52458333331020260100150000000000010019059.419059.4403800PROCESSED57541.50041666675419154515.85089120373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22025162Recovery operation of XIS CPU HALTCALIBRATION1ASWGNULLNULLNULLJAP2AO2XIS RECOVERY AND VERIFICATIONXISY
E0102.2-721916.0427-72.0346301.54252595-45.059285761.542954564.606388888954565.219027777810300101022361.52000022377.522361.5022377.5220210022318.522318.5529261PROCESSED57542.26917824075455754580.94097222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0204-72.038301.5525741-45.0563735246.600554622.160335648254622.855717592610300102021313200002132921313021329220210019486.919486.960069.90PROCESSED57542.73284722225455754636.32458333333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721915.987-72.0401301.56732456-45.05499026122.926554690.931574074154691.590555555610300103021301.82000021309.821309.8021301.8220210017083.117083.156929.90PROCESSED57543.27336805565455754710.28041666673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721915.9798-72.0267301.56915878-45.06851113190.543554761.105509259354761.626527777810300104025405.22000025405.225405.2025405.2220210022263.622263.645005.91PROCESSED57544.23170138895455754780.72311342593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0024-72.0211301.55876018-45.07361767248.527754813.564826388954814.3092476852103001050296182000029633.629634029618220210027676.927676.964293.90PROCESSED57544.94878472225455754839.99064814823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
E0102.2-721916.0385-72.0294301.54384101-45.06456362331.597854899.130486111154899.645428240710300106023843.92000023859.923843.9023867.9110110021711.221711.244463.90PROCESSED57545.74597222225455754916.36648148153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP313.989832.007275.70886169-8.5390255662.139354628.616481481554629.470312510300201033166.91000033166.933166.9033166.9330310029636.129636.173763.90PROCESSED57542.80190972225455754655.47825231483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP313.902331.877575.55993186-8.5644348221.265254811.222858796354811.857106481510300202021920.21000021920.221920.2021920.2220210019489.919489.9547700PROCESSED57544.71570601855455754826.35225694443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP (WIN FE)313.989832.007275.70886169-8.5390255662.139354628.616481481554629.470312510300301033166.92000033166.933166.9033166.9330310029636.129636.173763.90PROCESSED57542.81614583335455754655.4832870373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
CYGNUS LOOP (WIN FE)313.90231.877575.55976783-8.56423835221.264754811.857118055654812.432106481510300302026673.22000026673.226673.2026673.2220210022795.922795.949663.91PROCESSED57544.94415509265455754828.36791666673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
PERSEUS49.946841.518150.56975635-13.2575556686.816154691.60297453754692.620416666710300401040568.54000040584.540568.5040584.5220210031597.931597.987897.91PROCESSED57543.30519675935455754710.27644675933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
PERSEUS49.954641.5055150.58184418-13.26476244256.075954873.729861111154874.814108796310300402050006.64000050014.650014.6050006.6220210044840.444840.493669.90PROCESSED57545.55468755455754893.31336805563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
PERSEUS (1/4WIN)49.947541.518150.57020557-13.2572666686.815854692.620428240754693.107164351810300501021478200002147821501021486330310016992.216992.242049.90PROCESSED57543.29321759265455754780.52822916673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
PERSEUS (1/4WIN)49.955141.5057150.58205177-13.2643891255.65554874.814675925954875.439803240710300502028816.22000028816.228840.2028824.2330310026779.326779.3539860PROCESSED57545.52197916675455754893.01138888893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
RXJ1856.5-3754284.1503-37.908358.6012758-17.21588394280.508754759.797314814854761.097442129610300601043040.24000043048.243048.2043040.2220210037677.437677.41123220PROCESSED57544.24165509265455754780.52348379633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035001Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ksCALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP3AO3AO-3 XIS FLIGHT CALIBRATION PLANXISY
CRAB83.630822.0168184.5543577-5.7849163987.00554705.356145833354706.21891203710300701039822400003982239822039822220210032782.332782.374527.81PROCESSED57543.44402777785455754780.53518518523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035002We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP3AO3HXD CALIBRATIONS ON AO-3XISY
CRAB83.629522.0815184.49878495-5.7512948887.12554710.384456018554711.41266203710300801045090400004509045090045090220210033916.733916.788827.80PROCESSED57545.62880787045455754780.43864583333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035002We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP3AO3HXD CALIBRATIONS ON AO-3HXDY
LOCKMANHOLE162.936957.2546149.7046223253.2017902281.529654604.463530092654606.052939814810300901083419.78000083419.783419.7083419.7220210087485.287485.21373003PROCESSED57542.59214120375455754616.42065972223.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035002We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP3AO3HXD CALIBRATIONS ON AO-3XISY
PKS2155-304329.7153-30.227717.72680762-52.2446743458.230754598.570891203754599.112013888910301101023119200002311923119023119220210017813.117813.146745.90PROCESSED57542.51258101855455754608.99001157413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22035003XMM/Chandra/Suzaku cross calibration by an coordinated observation of PKS215-304.CALIBRATION1AISHIDAMANABUNULLNULLJAP3AO3COORDINATED OBSERVATION FOR CROSS-CALIBRATION WITH PKS2155-304XISY
CRAB83.635621.9544184.60973125-5.81455843269.396854923.074733796354924.041828703710400101042105.24000042808.542105.2042808.5220210033587.733587.783539.80PROCESSED57546.09012731485492254949.44586805563.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045003N/ACALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP4AO4CRAB CAL 2009HXDY
CRAB83.636322.0087184.56397797-5.78494551270.002155250.042719907455251.190497685210400107045830.94000045830.945830.9045830.93202100163181631899157.91PROCESSED57550.72805555565492255267.28466435183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045003N/ACALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP4AO4CRAB CAL 2009XISY
LOCKMAN HOLE162.937757.2549149.7037661453.20190951281.5354994.303935185254996.063437510400201092848.48000092848.492848.4092848.4220210079880798801520000PROCESSED57547.5745370375492255005.13898148153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045004HXD / XIS NXB/ CXB calCALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP4AO4LOCKMAN HOLE 2009XISY
LOCKMAN HOLE162.941957.2782149.6724024953.18794557110.36755161.431631944455161.75021990741040020202359.1120002383.12359.102375.1520310010017.410017.427515.90PROCESSED57549.57409722225492255182.65144675933.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045004HXD / XIS NXB/ CXB calCALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP4AO4LOCKMAN HOLE 2009XISY
PKS2155-304329.7145-30.226317.72895666-52.243833983.442354978.658321759354980.48640046310400401062440.16000062440.162440.1062440.1220210053071.753071.7157931.82PROCESSED57546.74568287045492254994.36212962963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045006This is a cross calibration observation with PKD2155-304 among Suzaku, XMM-Newton and Chandra.CALIBRATION1AISHIDAMANABUNULLNULLJAP4AO4CROSS CALIBRATION OF SUZAKU/XMM/CHANDRA WITH PKS2155-304XISY
E0102-7216.0343-72.0367301.54639234-45.0573719119.888554944.636956018554945.622510400501045028.72000045654.545028.7045654.5320310049726.949726.985135.81PROCESSED57546.2555492254966.35435185183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-7216.0181-72.0439301.55415549-45.0505370169.161155008.154409722255008.57108796310400601022061.52000022061.522061.5022061.5220210016326.316326.335991.91PROCESSED57547.6826620375492255022.24006944453.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-7215.9824-72.0274301.56809353-45.06775773194.758855130.759814814855131.416944444410400701020375.62000020383.620383.6020375.6220210018037.918037.956761.81PROCESSED57549.01152777785492255141.25027777783.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-7215.9813-72.0285301.56867985-45.06668362180.838655115.604803240755116.623761574110400801031449.92000031449.949641.1049935.3220210043716.743716.788013.91PROCESSED57548.86385416675492255134.43988425933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-7216.0091-72.0251301.55623091-45.06948422251.719355190.915983796355191.541192129610400901021985.22000021993.221985.2021993.2220210021639.621639.6540160PROCESSED57549.92961805565492255225.14693287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-7216.0186-72.0293301.55250278-45.06509107296.174555231.743506944455232.434305555610401001020500.62000020508.620500.6020508.6220210024497.124497.159675.92PROCESSED57550.47996527785492255249.72361111113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-72 1/4 WIN15.9806-72.0277301.56890722-45.06749655189.321455124.801620370455125.365428240710401101019091.32000019091.320038.1020038.13303100162091620948711.91PROCESSED57548.92784722225492255134.17777777783.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-72 1/4 WIN16.0261-72.0284301.54914583-45.06582801296.955655232.43515046355233.000277777810401201023553.72000023553.723553.7023560220210025339.425339.448815.90PROCESSED57550.49814814825492255266.23584490743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
E0102-72 PSUM15.9904-72.0242301.56429483-45.07078046218.004755166.902303240755167.933611111110401401062658.92000063019.262658.9063011.2120110054915.154915.189091.81PROCESSED57549.68570601855492255181.44063657413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISN
CYGNUS LOOP NE2313.943831.966775.6521583-8.5347761843.000554998.573240740754998.788344907410401501010889.71000010889.710889.7010889.722021009923992318577.90PROCESSED57547.57435185185492255008.10533564823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
CYGNUS LOOP NE2313.963431.956775.65508045-8.55396375223.000755175.792210648255176.064050925910401601012573.51000012573.512573.5012573.5110110010077.610077.623479.90PROCESSED57549.74635416675492255189.1156253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
CYGNUS LOOP P8313.995831.475275.29735897-8.8819537162.517354998.793078703754999.06688657411040170109708.7100009708.79708.709708.711011006711.96711.9236521PROCESSED57547.58081018525492255008.1510879633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
PERSEUS49.944441.5171150.56872595-13.2592973166.99855069.166990740755070.145300925910401801041279.84000041279.841279.8041295.8430310037348.837348.884499.81PROCESSED57548.3664120375492255088.12614583333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
PERSEUS49.951241.4934150.58651783-13.27626038277.324855228.335694444455229.250219907410401901038615.14000038615.138615.1038615.1220210035781.435781.478997.90PROCESSED57550.47075231485492255249.79850694443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
PERSEUS 1/4 WIN49.944441.516150.56934906-13.26021566.997655070.145312555071.50016203710402001055044.92000055067.755052.9055044.9330310051280.251280.2117049.82PROCESSED57548.37829861115492255109.41751157413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
PERSEUS 1/4 WIN49.950641.4949150.58528271-13.27525693276.944755229.25078703755229.707858796310402101021641.52000021649.121646.9021641.5330310021574.321574.3394820PROCESSED57550.4542129635492255249.71295138893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
RXJ1856.5284.1483-37.909358.59969969-17.21477781277.82955127.955011574155128.836342592610402201043484.54000043484.543492.5043492.5220210039424.639424.676101.80PROCESSED57548.96386574075492255141.28123842593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1AMATSUMOTOHIRONORINULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
RXJ1856.5284.0709-37.7784358.70367738-17.1102681979.474455269.457256944455270.685694444410402202040415.24000040426.940415.2040415.2220210034577.234577.2106107.90PROCESSED57550.90021990745492255285.08585648153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
RXJ1856.5284.1421-37.9072358.59959193-17.2095663977.586455281.152708333355282.371006944410402203042450.94000042450.942450.9042450.9220210011139.611139.61052522PROCESSED57551.05887731485492255301.29412037043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045007We propose some observations for the calibtaions of XIS.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP4AO4XIS FLIGHT CALIBRATION IN AO4XISY
G21.5-0.9278.3939-10.572821.49883061-0.89086145264.6555114.595798611155115.595300925910402301040156.14000040156.140156.1040156.1220210030452.130452.1863540PROCESSED57548.83776620375492255131.25196759263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22045008We propose G21.5-0.9 observation for the cross-calibtaions of XIS.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP4AO4CROSS CALIBRATION OF G21.5-0.9XISY
PKS2155-304329.7122-30.225117.73054892-52.2417270458.937255313.986817129655315.853645833310500101063457.26000063465.263471063457.2220210054701.554701.5161277.82PROCESSED57551.35295138895528755327.38160879633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055001This observation of PKS2155-304 is coordinated with XMM-Newton and Chandra.CALIBRATION1AISHIDAMANABUNULLNULLJAP5AO5COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTONXISY
CRAB83.638122.0079184.56555504-5.78396412269.479155291.525868055655292.5001273148105002010481.540000481.5481.60481.6220210033897.433897.484133.81PROCESSED57551.14728009265528755350.33689814823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055002We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP5AO5AO-5 CRAB CALIBRATIONXISY
LOCKMAN_HOLE162.938257.2507149.7086600153.20492954279.886955358.31187555360.082893518510500301077997.68000078013.677997.6078258.3220110073083.273083.2152981.81PROCESSED57552.05490740745528755370.33798611113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220550032010 Annual observation of Lockman hole, with XIS in the Psum mode.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP5AO5LOCKMAN HOLEXISN
E0102-7216.0161-72.0335301.55400478-45.06095473357.740555291.001469907455291.514745370410500401021592.82000021592.821592.8021592.81101100171391713944311.90PROCESSED57551.08263888895528755306.21443287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-7216.0035-72.0383301.55996349-45.0564353365.230855366.129641203755366.786979166710500402019230.22000019238.219238.2019230.2220210016589.516589.556783.92PROCESSED57552.38048611115528755413.40190972223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-7216.0129-72.0282301.55487873-45.06631044194.538955495.812569444455496.321793981510500404020018.92000020619.920018.9020643.9220210019219.319219.3439880PROCESSED57553.84841435185528755505.23028935183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-7216.0026-72.0263301.55918173-45.06842583227.092355539.025648148255539.48766203710500405020046.82000020070.820070.8020046.812020000039913.90PROCESSED57554.34619212965528755552.43599537043.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-7216.0173-72.0347301.55359992-45.05973194299.545755600.015243055655600.451631944410500406017242.62000017258.617242.6017258.6110110013743.213743.237695.90PROCESSED57600.86493055565528755617.40868055563.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-72_1_4_WIN16.0018-72.0347301.56035188-45.0600629565.865555366.787731481555367.309884259310500501020345.62000020353.620345.6020361.6220210017482.317482.3450802PROCESSED57552.37033564825528755400.42714120373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-72_1_4_WIN16.0156-72.0284301.55372169-45.06605315226.528555539.488368055655540.250254629610500502022538.82000022546.822538.8022554.833031005796.95796.965821.92PROCESSED57554.36627314825528755550.94366898153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
E0102-72_PSUM15.883-72.0319301.61184542-45.0653397966.388155367.310543981555368.5202314815105006010356.540000356.5356.50356.5110110030330336191.90PROCESSED57552.37533564825528755400.42995370373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISN
E0102-72_PSUM16.0136-72.0296301.55471109-45.06489883226.884455537.803437555539.025219907410500602040871.54000040936.340871.5041120.54301100157.4157.4105549.90PROCESSED57554.35957175935528755778.4332754633.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISN
E0102-72_PSUM16.0081-72.0302301.5571666-45.06441782138.522355437.76952546355438.888460648210500603037067.54000037083.137067.5037636.5220110033043.833043.896641.91PROCESSED57553.218755528755449.02615740743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISN
CYGNUS LOOP P8313.988531.481375.29810685-8.8732690362.518855358.013958333355358.301539351810500701012093.91000012881.612093.9012889.623021009985.59985.524839.90PROCESSED57551.9954745375528755376.42207175933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
CYGNUS LOOP P8 CI 6314.02131.464475.3027873-8.90540252222.299455552.962256944455553.04678240741050070202740100002755.6274002755.611011002487.42487.47295.90PROCESSED57554.49173611115528755593.25847222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
CYGNUS LOOP P8 CI 2314.008831.469175.29974588-8.89438689222.216555553.046979166755553.14469907411050070304963.1100004987497904963.112011003566.53566.58431.90PROCESSED57554.49218755528755593.26535879633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
RXJ1856.5-3754284.1491-37.9166358.59252855-17.21813017271.23955496.32953703755497.450972222210500801040091.74000040091.740099.7040107.7220210032908.132908.196875.80PROCESSED57553.87657407415528755509.06377314823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
PERSEUS49.940641.5199150.56470121-13.2585299866.58155417.382592592655418.01062510500901033624.24000033624.233624.2033624.2220210037659.637659.6542540PROCESSED57552.92643518525528755428.05931712963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
PERSEUS49.955741.5028150.58408011-13.26656036259.732555595.024942129655595.957847222210500902040461.14000040469.140461.1040477.1330310029594.329594.380593.91PROCESSED57600.84534722225528755610.2735879633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
PERSEUS_1_4_WIN49.940341.521150.56388564-13.2577360866.580555418.010636574155418.646747685210501001027372.72000027372.727380.4027386.4220210033712.733712.754955.91PROCESSED57552.92405092595528755428.07217592593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
PERSEUS_1_4_WIN49.955241.5037150.58324921-13.26601613259.96955594.462395833355595.024513888910501002021092.62000021096.321096.3021092.62202100165731657348559.90PROCESSED57600.82128472225528755610.26457175933.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
N132D81.279-69.6505280.31295018-32.7761326732.995455404.182129629655405.141122685210501101035849.53000035849.535849.5035849.5220210032540.932540.982839.81PROCESSED57552.73738425935528755414.10068287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055005We propose a observation of N132D for the calibration of the XIS in the AO5 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
CRAB_80OFF_0DEG83.695220.686185.71797799-6.4452152287.414955452.621446759355453.04671296310501201019241.52000019241.519241.5019241.5220210017364.417364.4367360PROCESSED57553.41087962965528755463.40942129633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_80OFF_22.5DEG83.152520.7619185.38009186-6.8334971886.920955453.047418981555453.491851851810501301018989.12000018989.118989.1018989.111011001372313723383760PROCESSED57553.41291666675528755463.41170138893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_80OFF_45DEG82.666321.0307184.90557346-7.0716184587.048255453.492557870455453.955011574110501401020599.22000020607.220607.2020599.2220210019812.119812.139937.92PROCESSED57553.42026620375528755463.41446759263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_50OFF_45DEG83.020221.413184.76043538-6.5876556487.675355431.833819444555432.068229166710501501010549.21000011277.210549.2011277.6220210010191.710191.720245.91PROCESSED57553.17444444445528755446.4468753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_50OFF_135DEG82.957622.5813183.73915584-6.006416486.656555432.069490740755432.31055555561050160106489.4100006489.46497.406497.422021003638.13638.1208220PROCESSED57553.17804398155528755446.44884259263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_50OFF_225DEG84.234422.6444184.32067652-4.9777683187.142755432.311585648255432.582777777810501701012345.61000012353.612345.6012361.61101100121511215123423.90PROCESSED57553.18753472225528755447.40869212963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_50OFF_315DEG84.296821.4693185.35120349-5.5532437387.174355432.583807870455432.898055555610501801014432.31000014432.314456.3014440.3110110012415.612415.627143.91PROCESSED57553.18938657415528755447.40998842593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_0DEG83.685920.9369185.49975653-6.3187471287.269655446.2555446.46054398151050190109657.5100009657.59657.509657.511011007899.57899.518183.90PROCESSED57553.31436342595528755461.39107638893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_45DEG82.848221.2156184.84096902-6.8289954886.960755446.461435185255446.68756944441050200109450.4100009458.49450.409458.422021007906.97906.919533.90PROCESSED57553.31466435185528755461.39252314823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_90DEG82.462921.9742184.00329077-6.7200094687.321155446.688553240755446.9076967593105021010109121000010921.910920010912220210010033.910033.9189300PROCESSED57553.31936342595528755461.39319444443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_135DEG82.761322.7517183.49649927-6.0665516287.03855446.908680555655447.13142361111050220109248.2100009248.29248.209248.222021007939.37939.319237.90PROCESSED57553.32697916675528755466.40063657413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_180DEG83.573923.1022183.60559643-5.2473007387.246655447.132268518555447.355729166710502301011470.61000011470.611478.6011478.6110110010091.310091.319295.90PROCESSED57553.32722222225528755461.39508101853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_225DEG84.392122.8458184.22714627-4.747488985.660855447.357129629655447.57934027781050240109404.2100009412.29404.209420.211011007822.57822.519191.90PROCESSED57553.32902777785528755461.39635416673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_270DEG84.796622.0949185.06495422-4.8283243886.316855447.580277777855447.7918287037105025010889110000889188910889111011008535853518273.90PROCESSED57553.33586805565528755461.39980324073.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
CRAB_65OFF_315DEG84.491321.2878185.60226135-5.495800987.605955447.793090277855448.02178240741050260101138210000113901139001138222021009884.19884.1197500PROCESSED57553.33793981485528755461.40040509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055006For better understanding of stray light levels we propose Crab offset observations for 180 ks in total.CALIBRATION1ATAKEIYOHNULLNULLJAP5AO5CALIBRATION OF STRAY LIGHTSPEY
PERSEUS_CI_649.957741.5001150.58689381-13.26798644252.245655614.208136574155615.18766203710502701045272.24000045905.545272.2045905.5220210041885.941885.984609.80PROCESSED57601.03800925935528755624.22494212963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
PERSEUS_1_4_WIN_CI_649.956541.5014150.58538691-13.26739774252.42755613.742210648255614.207800925910502801020636.32000020636.320636.3020636.31101100178451784540215.90PROCESSED57600.99693287045528755624.16398148153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055004We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP5AO5CALIBRATION OF X-RAY IMAGING SPECTROMETERXISY
CRAB83.635922.0094184.56318415-5.78488405269.619955641.813182870455643.1459490741105029010614.640000614.6614.60614.6220210036940.836940.8115139.90PROCESSED57601.32333333335528755652.16690972223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22055002We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV.CALIBRATION1ANAKAZAWAKAZUHIRONULLNULLJAP5AO5AO-5 CRAB CALIBRATIONXISY
LOCKMAN HOLE162.926557.2528149.7131534353.19882847305.989455685.740671296355686.767592592610600101042278400004227843590.5044442.7220110057821.457821.488709.80PROCESSED57601.95865740745565255768.81168981483.0.22.444Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISN
E0102-72 CI 615.9973-72.0342301.56226334-45.060657553.830755662.828449074155663.352256944410600201020386.23000020386.220386.2020386.22202100178421784245247.90PROCESSED57601.4698379635565255690.56906253.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
E0102-7216.0024-72.0368301.56029587-45.0579551869.544155741.097731481555741.582800925910600202028782300002879028798028782110110024611.524611.541903.91PROCESSED57602.43365740745565255775.2501504633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
E0102-7216.001-72.0295301.56019202-45.06526758183.159955848.646331018555849.090509259310600203032817.53000032825.532817.5032825.5220210029913.729913.738361.90PROCESSED57603.41947916675565255873.01065972223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
E0102-7216.0145-72.0334301.55469199-45.06108873340.238856003.383657407456004.16194444451060020403237830000323943237803239422021003071830718672440PROCESSED57604.95252314825565256019.27685185183.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
E0102-72 CI 215.9944-72.0366301.5637608-45.058324924.322855663.35296296355663.889074074110600205020814.32000020825.220822.2020814.3230210019623.919623.9463180PROCESSED57601.47387731485565255690.57054398153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN16.0104-72.0348301.55661541-45.059779734.797655663.889733796355664.409872685210600301016829.53000016829.518277.5018277.5220210016956.416956.444931.90PROCESSED57601.48619212965565255690.57133101853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN16.0013-72.0289301.56000261-45.06585975183.579755849.091076388955849.544664351810600302031657.13000031657.131753.1031769.1430310024464.324464.339183.90PROCESSED57603.42781255565255873.04267361113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8313.984131.488575.30130763-8.8657912262.516255721.291076388955721.583553240710600401011551.11000011559.111567.1011551.1110110010646.210646.225255.90PROCESSED57602.23280092595565255757.69432870373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8314.010131.455775.29000417-8.90377623240.002955915.057523148255915.319652777810600402011990100001199011990011990220210012321.212321.222643.90PROCESSED57604.15799768525565255932.0951620373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.943341.526150.56297877-13.2523263183.817355769.518888888955770.546793981510600501040838.24000040854.240838.2040963.1230210036688.536688.588801.91PROCESSED57602.70440972225565255792.32469907413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISN
PERSEUS49.953141.5016150.58309121-13.26863527261.998655964.847013888955965.916932870410600502046813.84000046813.846813.8046821.8320210045202.545202.592427.80PROCESSED57604.60072916675565256019.26645833333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
PERSEUS_CI_249.943941.5251150.56387356-13.2528295184.257555768.504976851855769.51827546310600601040145.34000040153.340161.3040145.3320210035470.335470.387505.90PROCESSED57602.69418981485565255792.23157407413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.943841.5162150.5688507-13.2602958567.732755796.23484953755796.716782407410600701020971.32000020971.321003.2020985.5230210018760.718760.741633.92PROCESSED57602.91091435185565255809.19670138893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.95441.5015150.58372556-13.26834695262.000955965.916944444455966.416782407410600702020856.92000020880.920872.9020856.9330310021425.521425.543173.91PROCESSED57604.59087962965565255991.45008101853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN_CI_249.942741.5184150.56689856-13.2589145567.730755795.757430555655796.23483796310600801023202.32000023210.323202.3023218.3320210022067.822067.8412440PROCESSED57602.90466435185565255806.34850694453.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1491-37.9147358.59438145-17.21743909269.059455856.46703703755857.32796296310600901039312.34000039312.339320.3039312.3220210035512.735512.774370.11PROCESSED57603.50932870375565255873.99760416673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
N132D81.27-69.6453280.30751952-32.78013136312.91455676.482893518555677.082013888910601001026045.32500026045.326045.3026045.32202100234212342151753.90PROCESSED57601.5851504635565255697.14476851853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
N132D81.2448-69.6458280.30994764-32.78867022111.825355841.444675925955841.870393518510601002023903250002390323903023903220210022252.922252.936763.90PROCESSED57603.34291666675565255858.37898148153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065001This is the proposal for the XIS calibration observations in the AO6 term.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP6AO6-CALXIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.71-30.218717.74059687-52.2391354958.796255677.090729166755678.592592592610601101060569.36000060577.360583060569.3320210049583.649583.6129709.81PROCESSED57601.63636574075565255697.23371527783.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065002This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories.CALIBRATION1AISHIDAMANABUNULLNULLJAP6AO6-CALCOORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTONXISY
CRAB83.629822.0234184.54825576-5.7821661487.102555805.247291666755806.2585532407106012010509.940000509.9509.90509.9220210036558.936558.987353.91PROCESSED57603.06591435185565255851.43533564823.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065003We propose to observe the Crab in order to calibrate the HXD response functions.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP6AO6-CALCALIBRATION OF HXD RESPONSE FUNCTIONSXISY
CRAB83.635722.0122184.56070723-5.78354183269.625455985.476574074155986.5585532407106013010521.740000521.7521.70521.7220210036421.736421.793465.81PROCESSED57604.78818287045565255995.24896990743.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065004We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP6AO6-CALCALIBRATION OF THE HXD RESPONSE FUNCTIONSXISY
CRAB83.635222.0094184.56283497-5.78543222269.699456000.005196759356001.1391435185106014010607400006076070607220210044787.944787.997955.81PROCESSED57604.93689814825565256019.33699074073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065004We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP6AO6-CALCALIBRATION OF THE HXD RESPONSE FUNCTIONSXISY
CRAB83.634822.004184.56721998-5.78863608269.698456012.546539351856013.5182407407106015010533.640000533.6533.60533.63202100245452454583940.91PROCESSED57605.06009259265565256023.26942129633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22065004We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP6AO6-CALCALIBRATION OF THE HXD RESPONSE FUNCTIONSXISY
LOCKMAN HOLE162.919757.2548149.7147987453.19475932318.694556052.890185185256053.675914351810700101035913.14000035933.735933.7035913.1110110034153.634153.667871.92PROCESSED57605.34888888895601856103.19978009263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISN
E0102-7216.0127-72.0346301.55559389-45.059930114.025856039.92609953756040.729421296310700201030438.23000030470.230438.2030462.2220210028052.828052.869401.90PROCESSED57605.24743055565601856054.26936342593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
E0102-7216.0126-72.0415301.55631435-45.0530488369.145956103.376828703756104.166805555610700202030726.93000030728.130726.9030728.1220210027423.627423.6682480PROCESSED57606.49929398155601856114.21019675933.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
E0102-7215.9776-72.0269301.57013713-45.06835815193.003256229.120717592656229.944641203710700203032102.6300003211032107.6032102.6220210029822.729822.771181.91PROCESSED57607.89122685185601856240.47508101853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
E0102-7216.0369-72.03301.54459754-45.06399958336.436456364.887071759356365.638344907410700204032601.33000032601.332609.3032609.3220210035668.735668.764895.90PROCESSED57610.79686342595601856377.51048611113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN16.0207-72.0344301.55208936-45.0599583914.018556040.729432870456041.552245370410700301032127.63000032127.632127.6032127.6220210029577.629577.6710861PROCESSED57605.2779745375601856068.62074074073.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN15.9774-72.0274301.57027283-45.06786356193.00456229.944652777856230.663425925910700302031357.13000031357.131357.1031357.1330310028574.328574.3621000PROCESSED57607.90833333335601856240.48356481483.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8313.985331.488475.30188904-8.8666439362.497556089.355428240756089.55230324071070040108222.1100008222.18222.108222.122021007339.47339.417007.91PROCESSED57605.63876157415601856106.17339120373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8314.009231.467575.29871729-8.89566896227.400756278.921273148256279.176493055610700402010045.61000010053.610061.6010045.62202100116821168222013.90PROCESSED57608.30059027785601856316.5364120373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.944841.5174150.56881272-13.258881972.610356159.979756944456160.982060185210700501041131.54000041131.541131.5041131.5220210038984.138984.186583.80PROCESSED57606.94086805565601856212.80251157413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.956241.5103150.58015129-13.26009762256.287656334.20827546356335.200752314810700502037690.14000041272.737690.1041522.1320210036431.436431.485733.80PROCESSED57610.58662037045601856349.58756944443.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.944341.5178150.56826526-13.2587546172.77756159.539351851856159.979421296310700601023678.62000023678.623678.6023678.61101100202552025538015.90PROCESSED57606.90127314825601856214.9810879633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.955641.5052150.582656-13.26459967255.901956335.201365740756335.687569444410700602022024.72000022032.722024.7022040.73303100177991779941999.91PROCESSED57610.58630787045601856349.57258101853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1441-37.9006358.60662879-17.2086350488.502456019.120914351856020.323738425910700701042087.74000042095.742087.7042095.7220210037740.337740.31039141PROCESSED57605.10780092595601856034.30146990743.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1491-37.909358.59994006-17.21536576268.999956220.582638888956221.757048611110700702044047400004404744047044047220210037256.837256.8101465.91PROCESSED57607.80373842595601856236.50895833333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
N132D81.2348-69.654280.32028023-32.79064068125.499356219.758553240756220.573738425910700801024141.62500024141.624141.6024141.62202100283822838270419.90PROCESSED57607.79275462965601856324.47190972223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
N132D81.2721-69.634280.29413666-32.78140611283.912156377.421539351856378.166956018510700802023118.22500023134.223118.2023134.2220210022472.522472.564397.91PROCESSED57610.92408564825601856387.49741898153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.7182-30.222817.73521081-52.24662805244.939456230.670798611156231.332777777810700901021377.12000021377.121377.1021377.1220210019998.319998.3571880PROCESSED57607.90538194445601856327.54849537043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075001This is the proposal for the XIS calibration observations in the AO7 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP7AO7XIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.7129-30.225517.73000788-52.2423720857.962856044.590717592656046.25016203710701001061887.26000061887.268199.2068199.2220210059298.659298.61433621PROCESSED57605.30368055565601856068.62180555563.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075002This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories.CALIBRATION1AISHIDAMANABUNULLNULLJAP7AO7COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTONXISY
CRAB83.630722.0167184.55439271-5.7850482387.681556196.232812556197.2258217593107011010520.240000520.2520.20520.222021003574835748857682PROCESSED57607.22866898155601856225.54679398153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075003We propose to observe the Crab in order to calibrate the HXD response functions.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP7AO7CALIBRATION OF HXD RESPONSE FUNCTIONSXISY
CRAB83.634222.0129184.55936471-5.78434175269.31256350.00859953756350.9133564815107012010515400005155150515330310039843.539843.578161.91PROCESSED57610.68753472225601856372.5489004633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075004We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP7AO7CALIBRATION OF THE HXD RESPONSE FUNCTIONSXISY
3C273187.28082.0495289.9587421364.35772193291.763756124.339513888956125.375208333310701301039755.34000039755.340363.3040359.6330310035778.335778.389475.82PROCESSED57606.64728009265601856141.1814004633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22075005This observation is a coordinated observation with NuStar, Chandra and XMM.CALIBRATION1AISHIDAMANABUNULLNULLJAP7AO7COORDINATED OBSERVATION OF 3C 273XISY
LOCKMAN HOLE162.944457.2754149.6743492653.19082755122.999656602.961863425956603.875115740710800101038846.34000038851.938846.3039095.2320210039473.639473.678901.91PROCESSED57613.24513888895638356652.68877314823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
E0102-7216.037-72.0354301.54508789-45.0586106118.198956409.460821759356410.234976851810800201029322.83000029344.829322.8029336.8110110046113.146113.166879.90PROCESSED57611.17660879635638356429.58623842593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
E0102-7216.0133-72.0418301.556039-45.0527345969.000756469.590243055656470.366203703710800202033138.33000033143.933141.4033138.32202100472784727867037.90PROCESSED57611.6439004635638356491.61174768523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
E0102-7215.986-72.0312301.5668942-45.06389041160.527456563.58702546356564.482094907410800203031959.53000031959.531959.5031961.5220210030139.430139.477317.90PROCESSED57612.75693287045638356625.63607638893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
E0102-7216.0359-72.0296301.54499373-45.06442014337.966356731.656678240756732.382175925910800204029279.33000029279.329279.3029287.3110110026418.826418.8626780PROCESSED57614.0235995375638356747.65791666673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN16.0332-72.0356301.5467628-45.058492918.202656410.234988425956411.005810185210800301027568.93000027568.930932.2030918.3220210047013.947013.966591.90PROCESSED57611.19752314825638356429.60673611113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN15.9825-72.0303301.56833182-45.06486245171.849856564.485578703756565.40640046310800302033612.93000033612.933612.9033612.9110110031660.931660.9795360PROCESSED57612.77995370375638356628.77261574073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8313.98331.489475.30140551-8.8644948762.296256450.973333333356451.367511574110800401011883.71000011892.711886011883.72202100129271292734055.91PROCESSED57611.4806255638356461.67069444443.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8314.008231.465275.29637267-8.89647626240.000156631.178425925956631.400868055610800402011768.31000011776.311768.3011784.311011008229.78229.719215.90PROCESSED57613.51674768525638356664.65556712963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.945941.5178150.56929207-13.2580940776.241956519.441134259356520.355833333310800501041256.9400004125741256.9041256.9320210040686.740686.7790061PROCESSED57612.27739583335638356587.7367129633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.954641.5052150.58201417-13.26501269255.999656693.526655092656694.38202546310800502037999.64000037999.637999.6037999.622020000000PROCESSED57613.79418981485638356709.70976851853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.946941.5176150.57004712-13.2578480775.899556520.356354166756520.809293981510800601021623.92000021623.921623.9021628.1220210018833.618833.639131.91PROCESSED57612.32800925935638356587.65927083333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.954541.505150.58206331-13.26522083255.999656694.38203703756694.788344907410800602018956.52000018974.318956.5018972.522020000000PROCESSED57613.79667824075638356709.71518518523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1435-37.9087358.59854994-17.2111410189.816456397.134791666756398.400949074110800701040747.34000040755.340747.3040755.322021003627236272109385.81PROCESSED57611.08035879635638356421.7048379633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1497-37.9108358.59836499-17.21646147268.997256570.388993055656571.604386574110800702040783.94000040831.940783.9040831.9220210035392.635392.6104997.80PROCESSED57612.85898148155638356628.79856481483.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
N132D81.2389-69.6575280.32407725-32.78861762111.49656571.613240740756572.17383101851080080205127.2250005127.25127.205127.2110110034963.134963.148423.91PROCESSED57612.84050925935638356628.76206018523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
N132D81.2957-69.6416280.30131329-32.77198365339.192456434.259155092656435.133460648210800803029839.42500029839.429859.4029847.42202100283352833575531.91PROCESSED57611.34646990745638356474.71659722223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
N132D81.229-69.6452280.31040291-32.79418529157.288456621.068680555656621.583495370410800804027046.82500027102.827046.80271101101100244302443044471.90PROCESSED57613.41684027785638356664.66376157413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
N132D81.2306-69.6358280.2992802-32.7953027210.999656668.911423611156670.97943287041080080507520.3250007520.37528.307528.3220200000124710PROCESSED57613.76712962965638356687.78072916673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.7186-30.226817.72877882-52.24740992244.69756595.140810185256595.676562510800901023765.12000023765.123765.1023765.1220210025583.625583.646283.90PROCESSED57613.1985995375638356608.61634259263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085001This is the proposal for the XIS calibration observations in the AO8 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP8AO8XIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.7149-30.226817.72820682-52.2442322258.756256405.840138888956407.378634259310801001053352.66000053352.653352.6053352.6220210048511.848511.8132923.82PROCESSED57611.20643518525638356608.62709490743.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085002This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories.CALIBRATION1AISHIDAMANABUNULLNULLJAP8AO8COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTONXISY
CRAB83.630722.0165184.5545625-5.785155387.299556565.417476851856566.4176273148108011010522.640000522.6522.60522.63202100401414014186405.90PROCESSED57612.8242129635638356588.56814814823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085003We propose to observe the Crab in order to calibrate the HXD response functions.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP8AO8CALIBRATION OF HXD RESPONSE FUNCTIONSXISY
CRAB83.634922.0126184.55996858-5.78395418269.569856722.056608796356723.0417939815108012010474.140000474.1474.10474.1320210032514.932514.985091.91PROCESSED57613.98982638895638356734.7060995373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085004We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP8AO8CALIBRATION OF THE HXD RESPONSE FUNCTIONSXISY
RX J1712.6-2414258.1492-24.2452359.865768418.7416922894.311856709.582395833356710.488333333310801401039713.34000039729.339713.3039729.3220210040442.740442.778255.81PROCESSED57613.89706018525638356754.67725694453.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22085006Check the change of PSF due to XRT heatter settingCALIBRATION1AMAEDAYOSHITOMONULLNULLJAP8AO8CONFIRMATION OF PSFXISY
E0102-7216.0411-72.0372301.54348026-45.0567266412.4956768.236006944456769.137696759310900101030737.53000030737.530745.5030745.522020000000PROCESSED57614.97127314825674856825.61773148153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
E0102-7215.984-72.028301.5674545-45.06712525192.497656958.321493055656959.232777777810900102028916.33000028916.332217.3032217.322020000000PROCESSED57616.70038194455674856986.39945601853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
E0102-7216.035-72.0314301.54556378-45.06264392356.211257115.673796296357116.459143518510900103029730.33000029730.329730.3029730.322020000000PROCESSED57617.91969907415674857183.6626620373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN16.0383-72.0354301.54452166-45.058582613.307556769.138541666756770.018182870410900201031670.83000031684.631670.8031684.622021007299729918287.90PROCESSED57614.98156255674856821.72665509263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
E0102-72_1_4_WIN15.9793-72.0266301.56936701-45.06862148192.503656959.232789351856960.093888888910900202023834.53000023834.531343.2031343.222020000000PROCESSED57616.70929398155674856979.43056712963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
E0102-72_PSUM16.041-72.0333301.54313775-45.06061925359.844157119.581076388957120.491736111110900301033311.33000033389.533397.5033311.322010000000PROCESSED57617.95034722225674857129.40646990743.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8313.984331.483775.29767156-8.8689790446.711256824.868761574156825.0675109004010934010000934093480934811011009797.19797.117167.90PROCESSED57615.25414351855674856835.71013888893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
CYGNUS_LOOP_P8314.005831.464675.29458482-8.89528015238.468356996.984745370456997.21543981481090040208889.3100008889.38889.308889.3110110093039303199281PROCESSED57617.45490740745674857092.19976851853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.943441.5178150.56768766-13.2591261567.343156896.672870370456897.18546296310900501019977.34000019977.320073.3020073.322020000000PROCESSED57616.52684027785674856910.64778935183.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
PERSEUS49.95641.5054150.5827994-13.26426763248.527357084.736747685257085.584953703710900502037204.64000037204.637204.6037204.632020000000PROCESSED57617.71309027785674857097.40442129633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
PERSEUS_1_4_WIN49.955641.5053150.58259934-13.26451625248.526457085.584965277857086.114120370410900601023649.22000023649.223649.2023649.211010000000PROCESSED57617.74653935185674857098.41414351853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
PERSEUS_PSUM49.956441.5056150.5829428-13.26393558248.527457086.114131944557086.775266203710900701030680.23000030680.230682.6030925.244021003903905390PROCESSED57617.73957175935674857098.01282407413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1438-37.9107358.59668979-17.2120890988.700156755.51297453756756.5002546296109008010389694000038969389690389692202100346213462185287.91PROCESSED57614.2257870375674856769.69971064823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
RXJ1856.5-3754284.1489-37.9089358.59997749-17.2151824269.168856953.687824074156954.815532407410900802039563.84000039563.839563.8039571.822020000000PROCESSED57616.68943287045674856979.41298611113.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
N132D81.2854-69.6352280.29457121-32.77663858305.054856764.201562556764.85430555561090090102492225000249222492202492222020000000PROCESSED57614.9606255674856782.49361111113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
N132D81.226-69.6524280.31905235-32.79393564136.005556960.098668981556960.557083333310900902013529.32500013529.324753.9024753.911010000000PROCESSED57616.71346064825674856979.43274305563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.721-30.225317.73158513-52.24930684244.750756960.565752314856961.291898148210901001020370.62000020370.621473.6021473.622020000000PROCESSED57616.73288194445674856979.44506944443.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095001This is the proposal for the XIS calibration observations in the AO9 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP9AO9XIS CALIBRATION OBSERVATIONSXISY
PKS2155-304329.7146-30.227817.72653709-52.2440841259.17556771.81672453756773.271006944510901101063991.66000063991.663999.6064009.422020000000PROCESSED57615.00471064825674856825.62120370373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095002This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories.CALIBRATION1AISHIDAMANABUNULLNULLJAP9AO9COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTONXISY
LOCKMAN HOLE162.940257.278149.6736799253.18739913107.872156991.012488425956991.993310185210901401037057.14000037057.137065.1037065.111011003920039200845480PROCESSED57617.45407407415674857006.96482638893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095005We observe the Locaman hole in order to calibrate the HXD background level.CALIBRATION1AFUKAZAWAYASUSHINULLNULLJAP9AO9CALIBRATION OF THE HXD RESPONSE FUNCTIONSXISY
SS CYG325.690743.576590.55960302-7.12368552237.982257010.266631944457010.997430555610901501043187.42000043187.443203.4043187.422020000000PROCESSED57617.54324074075674857049.45212962963.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095006ADDITIONAL CALIBRATION OF XRT WITH SS CYGCALIBRATION1AMAEDAYOSHITOMONULLNULLJAP9AO9XRT CHECK WITH SS CYGXISY
NEP270.034466.57496.3992847229.79775756142.516257052.938807870457056.250162037109016010154011.4200000000154011.400020000000PROCESSED57617.56754629635674857066.42177083333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095007MAINTENANCE OF SUZAKUCALIBRATION1ADOTANITADAYASUNULLNULLJAP9AO9NEPXISY
NEP270.035766.57496.3992847329.79724073142.516757056.250173611157056.725856481510901602021676.420000000021676.400010000000PROCESSED57617.57157407415674857066.42252314823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22095007MAINTENANCE OF SUZAKUCALIBRATION1ADOTANITADAYASUNULLNULLJAP9AO9NEPXISY
N132D81.2911-69.6367280.29591185-32.77442189319.851857144.691597222257145.540509259311000701031487.82500031487.831487.8031487.822020000000PROCESSED57618.0648379635711357164.528753.0.22.444Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22105001This is the proposal for the XIS calibration observations in the AO10 cycle.CALIBRATION1ATSUJIMOTOMASAHIRONULLNULLJAP10AO10XIS CALIBRATION OBSERVATIONSXISY
AE AQUARII310.0457-0.935545.22275468-24.45710482264.875953673.902268518553676.04327546340000101070528.910000070528.970616.970568.970544.9333310059453.859453.8184956.92PROCESSED57527.73082175935424754036.98513888893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001004We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.GALACTIC POINT SOURCES4ATERADAYUKIKATSUNULLNULLJAP0SWGSEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKUNULLN
AE AQUARII310.0612-0.93145.23545862-24.46836188250.624154033.231990740754034.382928240740000102047974.35000047974.348595.648131.648310.3222210045538.445538.499423.91PROCESSED57526.82387731485452654109.70834490743.0.22.439Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001004We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.GALACTIC POINT SOURCES4ATERADAYUKIKATSUNULLNULLJAP0SWGSEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKUHXDN
GX 349+2256.427-36.366349.145118412.7882060685.658453808.545324074153809.221678240740000301025230.85000025230.825233.225230.825230.8111110020050.720050.7584342PROCESSED57533.20063657415424754041.91320601853.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001026We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.GALACTIC POINT SOURCES4ATAKAHASHIHIROMITSUNULLNULLJAP0SWGSUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES)HXDN
GX 349+2256.4194-36.3657349.141664412.7932697778.935953813.926770833353814.604340277840000302028117.75000028117.728131.728120.428120.4222210025657.325657.3585380PROCESSED57533.27679398155424754042.16574074073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001026We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.GALACTIC POINT SOURCES4ATAKAHASHIHIROMITSUNULLNULLJAP0SWGSUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES)HXDN
SS CYG325.678943.573690.55119171-7.12024619276.578853676.050370370453676.985694444440000601039451.24000039451.239451.239451.239451.2222210032047.232047.2808101PROCESSED57527.71759259265424754036.98981481483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001043Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.GALACTIC POINT SOURCES4AISHIDAMANABUNULLNULLJAP0SWGSS CYG OBSERVATION IN QUIESCENCENULLN
SS CYG325.684243.573990.55430501-7.12254626256.876753692.606620370453693.8646759259400007010560436000056059561795604356059222210054357.254357.2108665.82PROCESSED57528.04357638895424754037.91284722223.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001044Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.GALACTIC POINT SOURCES4AISHIDAMANABUNULLNULLJAP0SWG-TOOSS CYG OBSERVATION IN OUTBURSTXISN
X1630-472248.4828-47.3401336.939147190.2980170978.334153774.631898148253775.139097222240001001022190.220000022190.222190.222190.222190.211111002224722247438160PROCESSED57532.93807870375424754040.95408564823.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001058We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLJAP0SWG-TOOFE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIESHXDN
X1630-472248.4706-47.343336.931406960.3021212969.065753781.979108796353782.54743055564000100202142920000021429214852142921429222210017022.317022.349101.90PROCESSED57533.01175925935424754041.48920138893.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001058We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLJAP0SWG-TOOFE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIESHXDN
X1630-472248.4772-47.3405336.936278280.3005330675.595953794.970833333353795.696805555640001003021521.620000021521.621521.621521.621521.6222210019032.819032.8627180PROCESSED57533.10790509265424754041.59560185183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001058We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLJAP0SWG-TOOFE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIESHXDN
X1630-472248.5414-47.3441336.963141370.26612574120.577553802.075879629653802.730023148240001004021248.120000021248.121249.921249.921249.9333310020477.820477.8565120PROCESSED57533.16204861115424754041.76987268523.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001058We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLJAP0SWG-TOOFE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIESHXDN
X1630-472248.5239-47.3401336.958040410.27755382107.661653809.22641203753809.74391203740001005023167.120000023175.123176.923176.823167.1212210018860.518860.5447060PROCESSED57533.21899305565424754041.93026620373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001058We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLJAP0SWG-TOOFE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIESHXDN
X1630-472248.5405-47.3458336.961478290.2654214120.353817.426030092653817.931342592640001006021654.120000021662.121654.121654.121654.1212210022761.922761.943655.91PROCESSED57533.30337962965424754042.10432870373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001058We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLJAP0SWG-TOOFE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIESHXDN
4U1626-67248.0601-67.4675321.78071552-13.09322804103.035953803.054351851853805.818275463400015010102639.2100000102654102639.2102647.2102654222210093393.293393.2238781.93PROCESSED57533.23496527785424754042.46636574073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001081The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase,GALACTIC POINT SOURCES4AANGELINILORELLANULLNULLJAP0SWG4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINEXISN
CH CYG291.162150.242481.8655065215.56609243185.748153739.573645833353740.291956018540001602033305.82500033307.533337.833315.533305.8222210028461.528461.5620561PROCESSED57532.63559027785424754039.67122685183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001082CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS.GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLJAP0SWGSUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNIXISN
CH CYG291.116850.249481.8599702815.5954142438.186153883.311296296353884.15021990744000160303514435000351523516035160351441111100374593745972447.91PROCESSED57534.45737268525425854109.70439814823.0.22.439Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22001082CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS.GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLJAP0SWGSUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNIXISN
JUPITER226.5694-16.1887343.9653677835.7224308118.490153790.764340277853791.794027777840100101037759.43600037767.437759.437767.437767.4222210032836.132836.188936.11PROCESSED57533.07815972225440153905.5339004633.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011003We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.GALACTIC POINT SOURCES4CELSNERRONALDNULLNULLUSA1AO1JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUMXISN
JUPITER226.5948-16.1928343.9861341935.70433361118.490653791.794131944553792.7940277778401001020377043600037704377043770437704111110032778.132778.1863601PROCESSED57533.09439814825440153905.50354166673.0.22.436Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011003We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.GALACTIC POINT SOURCES4CELSNERRONALDNULLNULLUSA1AO1JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUMXISN
JUPITER226.6157-16.1957344.0035670735.68981432118.490753792.794085648253793.859942129640100103040791.23600040799.240791.240799.240799.2222210035536.335536.392073.90PROCESSED57533.10630787045440153905.58680555563.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011003We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.GALACTIC POINT SOURCES4CELSNERRONALDNULLNULLUSA1AO1JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUMXISN
JUPITER226.6349-16.1983344.0196225935.67652355118.490853793.8653794.958553240740100104042255.83600042263.842263.842263.842255.8222210035706.735706.794905.92PROCESSED57533.11038194445440153906.57126157413.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011003We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure.GALACTIC POINT SOURCES4CELSNERRONALDNULLNULLUSA1AO1JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUMXISN
XB1323-619201.6454-62.1418307.024981820.4503340299.573154109.479490740754110.916840277840100201055936.85000055936.855936.8055936.8220210081817.381817.3124176.91PROCESSED57536.86660879635473554133.02717592593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010002XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting.GALACTIC POINT SOURCES4CDOTANITADAYASUNULLNULLJAP1AO1BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619XISY
SS 433287.95314.990639.69950989-2.237940978.644553829.610960648253830.532766203740100301038676.74000038676.738676.738676.738676.7222210028241.128241.1796341PROCESSED57533.3951620375439453906.14781253.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010031SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.GALACTIC POINT SOURCES4AKAWAINOBUYUKINULLNULLJAP1AO1SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGEXISN
SS 433287.95274.9939.69879316-2.2378642778.644653833.461145833353834.457916666740100401040197.64000040221.640197.640229.640213.6222210030474.930474.9861102PROCESSED57533.43576388895440053906.55017361113.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010031SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber.GALACTIC POINT SOURCES4AKAWAINOBUYUKINULLNULLJAP1AO1SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGEXISN
G11.2-0.3272.867619.43346.3458611617.2973811977.643253834.462604166753835.663414351840101001043984.65000043992.643984.643992.643992.6222210037387.937387.983679.91PROCESSED57533.42791666675439753905.46718753.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010049The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU.GALACTIC POINT SOURCES4CHAYATOASAMINULLNULLJAP1AO1CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3XISN
CYGNUS X-3308.259340.98179.932302990.62160244252.42454052.090289351854054.367638888940101101099744.510000099746.299746.2099744.5220210095389.395389.31967451PROCESSED57536.15207175935445654088.95450231483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010058We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3.GALACTIC POINT SOURCES4CKITAMOTOSHUNJINULLNULLJAP1AO1WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKUSPEY
LMC X-280.025-71.9941283.14092563-32.7117801313.302253849.38171296353850.7731365741401012010561526000056165.756165.7561525616022221007340873408120193.81PROCESSED57533.57353009265439453907.62880787043.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010090We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not.GALACTIC POINT SOURCES4BTAKAHASHIHIROMITSUNULLNULLJAP1AO1DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2HXDN
SGR1806-20272.1595-20.34910.0481975-0.2082305388.748354189.630555555654190.062719907440102101019288.92000019288.919595019356.3110110016507.116507.137327.91PROCESSED57538.02535879635456154209.51692129633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010124We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.GALACTIC POINT SOURCES4ANAKAGAWAYUJINNULLNULLJAP1AO1-TOOPROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"HXDN
SGR1900+14286.8039.387543.075949620.8014990786.553353826.363159722253826.911331018540102201017056.22000017704.621707.421655.517056.2121110014360.414360.4473361PROCESSED57533.348755439453906.09778935183.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010124We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs.GALACTIC POINT SOURCES4ANAKAGAWAYUJINNULLNULLJAP1AO1-TOOPROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR"HXDN
HESS J1837-069279.4395-6.865125.2664546-0.10276403102.614454164.534189814854165.428634259340102601042191.14000042191.142199.1042207.1220210037702.137702.177259.91PROCESSED57537.60101851855475054171.26134259263.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22010131The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP1AO1INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRALHXDY
1E1207.4-5209182.5062-52.436296.54584039.92149786302.493953946.568206018553948.260358796340103001096351.912000096351.9102278.496367.996351.9323310094049.894049.8135379.91PROCESSED57535.12307870375475054132.81872685183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220101521E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.GALACTIC POINT SOURCES4BYOSHIDAATSUMASANULLNULLJAP1AO1A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209XISN
1E1207.4-5209182.4916-52.442296.537914819.91413144148.689354146.208738425954147.639050925940103002049826.65000050073.449826.6050089.4120110044446.844446.81235762PROCESSED57537.43723379635475054153.98864583333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220101521E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object.GALACTIC POINT SOURCES4BYOSHIDAATSUMASANULLNULLJAP1AO1A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209XISY
AB DOR82.2835-65.427275.26967334-33.00819219154.677454060.026527777854061.458611111140103101053451.78000053451.753459.7053461.4220210048033.448033.41237081PROCESSED57536.1704629635450254133.02229166673.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011021We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku.GALACTIC POINT SOURCES4BAUDARDMARCNULLNULLUSA1AO1NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARESHXDN
AB DOR82.2881-65.4658275.31538375-33.00189818204.284954108.064756944454109.472442129640103102049096.54500049096.549096.5049096.5220210044961.144961.1121619.92PROCESSED57536.50005787045450254133.01270833333.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011021We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku.GALACTIC POINT SOURCES4BAUDARDMARCNULLNULLUSA1AO1NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARESHXDN
HR 9024357.412536.4308109.27773456-24.7972906849.862453939.061678240753940.601608796340103201058775.76000058799.758775.758783.758791.7222210056011.656011.6133039.81PROCESSED57535.0420254635440153950.26240740743.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011022Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions.GALACTIC POINT SOURCES4BTESTAPAOLANULLNULLUSA1AO1GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARSXISN
SIGMA^2 CRB243.655233.788154.5640236446.14689859281.120753969.476446759353972.1925231482401034010109160.4110000109190.4109160.4109168.4109176.4222210098837.698837.6234653.93PROCESSED57535.38777777785452654021.25785879633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011025Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD.GALACTIC POINT SOURCES4BBROWNALEXANDERNULLNULLUSA1AO1SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEMHXDN
BETA LYR282.509433.373863.1946287614.7959456959.470453862.54547453753862.995208333340103601020251.52000020267.520251.520267.520267.522221009894.79894.738851.91PROCESSED57533.73942129635440153913.81915509263.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011031The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA1AO1AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAEXISN
BETA LYR282.509833.371663.1926692414.7947785353.497453867.126018518553867.625219907440103602021496.22000021496.221496.221496.221496.2111110019164.219164.243119.92PROCESSED57534.27648148155440153914.27841435183.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011031The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA1AO1AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAEXISN
BETA LYR282.509333.371963.1927860914.7952801253.497353871.431122685253871.857187540103603018195.42000018195.418195.418195.418195.4222210019842.119842.136807.90PROCESSED57534.31605324075440153920.41643518523.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011031The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA1AO1AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAEXISN
1RX J154814.5-452845237.0511-45.4226332.469613937.0704069785.735854132.636851851854135.354386574140103701099454.110000099454.199462.1099470.1220210086855.286855.2234783.83PROCESSED57537.02527777785470254139.47679398153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011102Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber.GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLUSA1AO1BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTIONHXDY
1RXS J213344.1+51072323.435451.197394.50909334-0.4244770594.045253854.285300925953856.250173611140103801081924.18000081924.181924.181924.181924.1222210062888.162888.1169726.13PROCESSED57533.63306712965439153908.18879629633.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011102Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber.GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLUSA1AO1BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTIONHXDN
V893 SCO243.8144-28.6275348.0657733615.88028883274.674653973.402418981553974.05641203740104101018497.82000018497.818497.818497.818497.8222210016140.316140.3564820PROCESSED57535.36956018525452654053.47638888893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011103The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies.GALACTIC POINT SOURCES4BMUKAIKOJINULLNULLUSA1AO1CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAEXISN
T CRB239.877325.910642.3602798548.16117824268.932153984.947465277853986.091192129640104301046303.35000046311.346311.346319.346303.3222210045431.445431.498815.91PROCESSED57535.51071759265452654053.43408564823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011106Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism.GALACTIC POINT SOURCES4ASOKOLOSKIJENNIFERNULLNULLUSA1AO1THE NATURE OF HARD X-RAY SYMBIOTIC BINARIESXISN
4U 1705-44257.2295-44.1004343.32321952-2.34240238264.079453976.242916666753976.773171296340104601018315.52000018315.518315.518315.518315.5222210015371.515371.545809.90PROCESSED57535.38892361115452654021.3060879633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011112We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.GALACTIC POINT SOURCES4AYOUNGANDREWNULLNULLUSA1AO1REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44XISN
4U 1705-44257.2281-44.1019343.32141433-2.34248879264.066653996.517361111153996.8619675926401046020171342000017342171341733417334111110015447.715447.729767.90PROCESSED57535.60821759265452654020.90555555563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011112We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.GALACTIC POINT SOURCES4AYOUNGANDREWNULLNULLUSA1AO1REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44XISN
4U 1705-44257.2313-44.1028343.32206131-2.34487049297.079354014.424270833354015.0891087963401046030200652000020065200652006520065222210017919.617919.657423.92PROCESSED57535.79451388895452654021.67651620373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011112We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state.GALACTIC POINT SOURCES4AYOUNGANDREWNULLNULLUSA1AO1REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44XISN
4U 1820-30275.9207-30.36232.78792233-7.91550172265.975453992.923460648253993.660590277840104701025700.83700025700.825810.925723.925714.8212210031878.231878.263633.91PROCESSED57535.60129629635452654021.22270833333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011113The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.GALACTIC POINT SOURCES4BMILLERJONNULLNULLUSA1AO1A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIESXISN
SERPENS X-1279.99345.028536.113117894.83561165256.142354032.285381944454033.225914351840104801037157.83700037157.837269.837205.837165.8212210031069.531069.581239.92PROCESSED57535.97347222225452654056.47193287043.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011113The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.GALACTIC POINT SOURCES4BMILLERJONNULLNULLUSA1AO1A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIESXISN
CYGNUS X-2326.165338.332387.3318132-11.304984776.314253871.863680555653872.729317129640104901039390.33700039390.339406.339390.339390.3212210036880.436880.4747861PROCESSED57534.38582175935440153927.64291666673.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011113The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme.GALACTIC POINT SOURCES4BMILLERJONNULLNULLUSA1AO1A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIESXISN
4U 1636-536250.2262-53.7541332.91086545-4.8175149191.245754140.387754629654140.9912540105001024232190002423224232024232210210021689.521689.5521360PROCESSED57537.34100694455452554151.50528935183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011117Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.GALACTIC POINT SOURCES4AHOMANJEROENNULLNULLUSA1AO1THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536XISY
4U 1636-536250.2273-53.7542332.91122007-4.8180699991.244754153.295578703754154.3544560185401050020400963800040096401040400962102100355503555091477.90PROCESSED57537.48219907415452554158.3920370373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011117Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.GALACTIC POINT SOURCES4AHOMANJEROENNULLNULLUSA1AO1THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536XISY
4U 1636-536250.2272-53.754332.91133194-4.8178937291.245454160.042442129654160.893159722240105003038719.33800038727.438719.3038719.4210210048145.948145.9734981PROCESSED57537.51611111115469554167.64004629633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011117Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.GALACTIC POINT SOURCES4AHOMANJEROENNULLNULLUSA1AO1THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536XISY
4U 1636-536250.2277-53.7538332.91167841-4.8179842993.244554186.480277777854187.304328703740105004032130.43800032130.432138.4032130.4210210027784.227784.271177.91PROCESSED57538.01417824075469554209.5414120373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011117Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.GALACTIC POINT SOURCES4AHOMANJEROENNULLNULLUSA1AO1THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536XISY
4U 1636-536250.2259-53.7533332.911352-4.8168543100.775554188.472071759354188.785694444540105005012241.83800012249.812241.8012249.821021001180411804270880PROCESSED57537.99731481485469554200.46877314823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011117Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle.GALACTIC POINT SOURCES4AHOMANJEROENNULLNULLUSA1AO1THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536XISY
4U 1822-37276.4461-37.1042356.85149319-11.29112534258.453754010.456388888954011.518969907440105101037743.44000037768.237768.237743.437743.4222210033178.533178.591805.90PROCESSED57535.76153935185469554024.65398148153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011121We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe.GALACTIC POINT SOURCES4BCOTTAMJEANNULLNULLUSA1AO1ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37XISY
IGRJ16465-4507251.6303-45.1738340.003433380.10772124284.956253987.383981481553987.920300925940105201022527.92000022535.922527.922535.922535.9222210024645.424645.4463320PROCESSED57535.49759259265452654021.1132870373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011132INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA1AO1HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYSHXDN
SWIFTJ2000.6+3210300.086932.203368.995708361.144314787.423353837.661921296353837.913935185240105301012438.4200001244412451.212451.212438.411111009876.79876.721767.90PROCESSED57533.44561342595477553927.35491898153.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011132INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA1AO1HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYSHXDN
SWIFTJ2000.6+3210300.113732.121868.938355011.08211502255.607254039.020567129654039.302997685240105302012748.41000012756.412748.412756.412756.42222100117271172724393.90PROCESSED57535.98594907415477554056.19599537043.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011132INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA1AO1HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYSHXDY
IGRJ16493-4348252.3173-43.8652341.319117580.57823277287.44454013.882291666754014.420416666740105401021199.82000021215.821215.821199.821207.8333310020219.720219.746463.91PROCESSED57535.78186342595469554025.47964120373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011132INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA1AO1HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYSHXDY
SWIFTJ1010.1-5747152.7309-57.8539282.8705066-1.37559689290.701253891.217553891.554456018540105501019171.72000019171.719171.719171.719171.7222210017877.817877.829087.90PROCESSED57534.49069444445440153926.10753472223.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011132INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA1AO1HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYSHXDN
IGRJ16195-4945244.8541-49.816333.491170840.29973526284.030153998.850833333353999.723148148240105601039148.64000039148.639148.639148.639148.6222210042265.242265.275357.91PROCESSED57535.6526620375452654020.92271990743.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011132INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA1AO1HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYSHXDN
4U1907+09287.40139.837843.747393140.4853172760.259953857.258032407453858.732222222240105701058440.36000058440.358456.358448.358456.3222210038821.538821.5127353.91PROCESSED57533.66905092595440153913.43674768523.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011133We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA1AO1THE BROAD BAND SPECTRUM OF 4U1907+09XISN
4U1700-37255.9894-37.8441347.755821022.17172645269.694553991.44766203753992.91891203740105801081442.58000081456.981470.481442.581454.4333310082109.382109.31271091PROCESSED57535.60979166675452654053.54282407413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011135The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse.GALACTIC POINT SOURCES4AKALLMANTIMOTHYNULLNULLUSA1AO1IRON LINE VARIABILITY IN 4U1700-37XISN
CYGNUS X-1299.612435.13371.285775563.01567368256.220254038.150127314854038.822540105901027706.83000027706.827737.827706.827706.8212210027689.227689.258083.90PROCESSED57535.99497685185452654063.49248842593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011141We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.GALACTIC POINT SOURCES4BNOWAKMICHAELNULLNULLUSA1AO1ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERAHXDN
GX 339-4255.7025-48.7916338.93635594-4.3258796686.748954143.231608796354146.200300925940106801077205.310000083893.577205.3082113.8220210094026940262564844PROCESSED57537.49052083335453554167.77518518523.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22011146Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme.GALACTIC POINT SOURCES4AMILLERJONNULLNULLUSA1AO1-TOOSUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURSTXISN
SGR 1806-20272.166-20.47299.94279657-0.27364584269.947353987.926192129653989.166828703740109201048915.55000048915.548923.548931.548931.5111110055408.555408.5107175.91PROCESSED57535.52724537045452654021.11126157413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22012017The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters.GALACTIC POINT SOURCES4BMEREGHETTISANDRONULLNULLEUR1AO1COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLAREHXDN
ALGOL47.083140.8965149.0355551-14.93487401244.477154167.619722222254169.6132986111401093010102164.2105000102164.2102164.20102164.22202100102472.9102472.9172192.81PROCESSED57537.68258101855473654186.39835648153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22012024Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD.GALACTIC POINT SOURCES4CGUEDELMANUELNULLNULLEUR1AO1A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOLHXDY
IGR J16318-4848247.9691-48.8061335.63186461-0.44896472266.594853961.482553964.348831018540109401097253.810000097269.897253.897269.897269.8222210087112.887112.8247605.95PROCESSED57535.34835648155452654020.91815972223.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22012034We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848.GALACTIC POINT SOURCES4BWILMSJOERNNULLNULLEUR1AO1OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTIONXISN
XB 1916-053289.7027-5.241531.35614078-8.46800846250.253854047.24297453754048.111979166740109501038464.74000039096.739088.738464.739096.7222210037485.737485.7750822PROCESSED57536.06842592595473554088.8660879633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22012038We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV.GALACTIC POINT SOURCES4ADIAZ TRIGOMARIANULLNULLEUR1AO1BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBSXISY
HESS J1731-347263.0179-34.7706353.53173388-0.6819800579.800554154.780706018554155.743229166740109901040618.93800040626.940618.9040626.9220210034647.934647.983155.90PROCESSED57537.47393518525452854160.39319444443.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22012042The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator.GALACTIC POINT SOURCES4APUEHLHOFERGERDNULLNULLEUR1AO1THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347XISN
1E 1841-045280.3141-4.873527.43528490.0368680277.322753844.452546296353847.132800925940110001097962.210000097962.297970.297970.997970.922221006347463474231539.92PROCESSED57533.57480324075440153907.28065972223.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22014204Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data.GALACTIC POINT SOURCES4AHARRUSILANANORIIMIKIOUSJ1AO1SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73HXDN
HESSJ1813-178273.3946-17.770412.870145030.0115547390.936754160.899976851854162.281469907440110101063839.16500063847.163839.1063847.1220210057756.157756.1119351.91PROCESSED57537.53584490745473654167.63469907413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22014214Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies.GALACTIC POINT SOURCES4BREIMEROLAFEBISAWAKENUSJ1AO1IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE?HXDY
EX HYA193.0706-29.2994303.1528895233.57198642300.000454299.891215277854302.4377199074402001010100515.7100000100523.7100515.70100523.7220210091113.591113.5219959.91PROCESSED57539.33190972225470754339.51394675933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020008The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS.GALACTIC POINT SOURCES4AISHIDAMANABUNULLNULLJAP2AO2MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARSHXDY
V1223 SGR283.7445-31.1055.0082738-14.3198720579.952854203.480324074154204.941805555640200201060706600006070660706060706220210046286.146286.1126271.92PROCESSED57538.18228009265474454210.65968753.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020008The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS.GALACTIC POINT SOURCES4AISHIDAMANABUNULLNULLJAP2AO2MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARSHXDY
1RXSJ174459.5-172640266.2467-17.44069.769581816.08973572101.046154555.630405092654556.583495370440200301043579.34000043595.343579.3043603.3110110029591.629591.682343.91PROCESSED57541.99754629635493754570.15292824073.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020015We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates.GALACTIC POINT SOURCES4CMORIHIDEYUKINULLNULLJAP2AO2SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ165256.3-264503253.236-26.7533355.142008510.81079439277.587654337.002442129654338.041944444440200401049582.24000049582.249582.2049582.2220210046658.146658.189777.92PROCESSED57539.67770833335472354350.41550925933.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020015We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates.GALACTIC POINT SOURCES4CMORIHIDEYUKINULLNULLJAP2AO2SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXS J070407.9+26250106.034126.4126190.2749702514.29877104282.071754548.486886574154549.986238425940200801058315.75000058323.758315.7058323.7110110049476.649476.6129527.80PROCESSED57541.98089120375493354566.3267129633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020029Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically.GALACTIC POINT SOURCES4CISHIDAMANABUNULLNULLJAP2AO2OBSERVATIONS OF SOFT INTERMEDIATE POLARSXISY
1RXS J180340.0+40121270.93240.209866.858344225.77561005157.53854478.029097222254479.187777777840200901053090.75000053090.753090.7053090.7110110044348.944348.9100095.93PROCESSED57541.29656255486454490.07072916673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020029Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically.GALACTIC POINT SOURCES4CISHIDAMANABUNULLNULLJAP2AO2OBSERVATIONS OF SOFT INTERMEDIATE POLARSXISY
4U 0142+6126.480361.7944129.32255084-0.3994607640.95954325.169594907454327.520925925940201301099674.410000099674.499674.4099674.42202100101609.6101609.6203129.74PROCESSED57549.8239004635473054347.62212962963.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020058Recently, high energy pulsed x-ray emissions from anomalous x-ay pulsears have been founded. This emissions extend to neary 100 keV with photon index ~1, and the emission mechanism is unknown. In order to trace this enigmatic component, we propose the observation of the anomalous x-ray pulsar 4u 0142+61 with 100 ksec exposures. The main aim of this observation is to examine how high energy this emission extend to. Because the these emissions are almost 100% pulsed component, so using the pulse on-off method, we can achive the ultimate sensitivity not depending on the reproducibility of the background but depending only on the photon statistics. If the spectrum have the strong break neary ~250 keV, this emissions have originated as the compton scatterd photons in the star surface.GALACTIC POINT SOURCES4AENOTOTERUAKINULLNULLJAP2AO2THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61HXDY
PSR B1259-63195.6821-63.8856304.1741357-1.04108664280.93554288.62202546354289.06266203740201401021863.42000021871.421863.4021871.41101100268602686038063.91PROCESSED57539.12564814825469654328.48847222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6782-63.8867304.17237227-1.04211039282.653454290.685208333354291.187604166740201402019481.72000019481.719481.7019481.7220210026911.126911.1433781PROCESSED57539.13967592595469654328.50320601853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6777-63.8873304.1721261-1.04270018282.652754292.629131944454293.191076388940201403022721.72000022721.722721.7022721.7220210024280.824280.848545.90PROCESSED57539.16067129635470754339.02738425933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6732-63.8823304.17036556-1.03761834285.894554294.656886574154295.345995370440201404022914.92000022914.922914.9022914.9220210021070.621070.659495.91PROCESSED57539.26512731485470954339.41425925933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6556-63.8839304.16255435-1.03887935293.483254304.281122685254304.687777777840201405019702.32000019702.319702.3019702.3110110017754.917754.935127.90PROCESSED57539.30247685185470754339.21753472223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6402-63.8787304.15600524-1.03339065289.999254315.264085648254316.041944444440201406024038.82000024038.824038.8024038.8220210021580.821580.867195.91PROCESSED57539.39696759265472254347.69465277783.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6594-63.8834304.16424752-1.0384525292.999854330.058148148254330.687777777840201407020481.22000020481.220481.2020482.9220210019470.319470.3543640PROCESSED57539.65472454356.22284722223.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
PSR B1259-63195.6089-63.8685304.14267075-1.0226082321.933354348.230844907454348.604328703740201408018332.72000018340.718348.7018332.7110110022351.322351.3322600PROCESSED57539.92714120375472454356.19995370373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020059We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLJAP2AO2THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63HXDY
LS 5039276.5633-14.910916.82651822-1.31880921270.41254352.678055555654358.4725402015010203239.9200000203239.9203239.90203239.92202100181095181095442087.94PROCESSED57540.09476851855474554384.72590277783.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020062The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system.GALACTIC POINT SOURCES4ATAKAHASHITADAYUKINULLNULLJAP2AO2SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039HXDY
HETEJ1900.1-2455285.0506-24.980211.25454685-12.90928139259.419254389.591342592654390.507106481540201601041759.14000041778.841759.1041775.1220210039906.339906.379105.81PROCESSED57540.31585648155477154403.12927083333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020068We propose a 40 ks observation of the accreting millisecond pulsar HETE J1900.1-2455, which was discovered by HETE-2 only recently. Good sensitivity in 10-100keV and enough timing resolution of HXD on Suzaku allow us to measure the light curve and the phase resolved spectra of its hard X-ray pulsation, with which we study the physical parameters of the Comptonizing plasma that is considered as the source of the hard X-ray emission of accreting millisecond pulsars. With XIS, we study the radiation from the accretion disk and the neutron star surface, and search for spectral features such as emission lines or absorption edges, which will provide information on the binary environment.GALACTIC POINT SOURCES4BSUZUKIMOTOKONULLNULLJAP2AO2HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455HXDY
4U 1700+24256.631623.907145.0741901132.98144858280.14954334.778761574154335.87516203740202301050244.55000050252.550260.5050244.5220210045326.845326.894715.82PROCESSED57539.66362268525472354350.46064814823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020105We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV.GALACTIC POINT SOURCES4BNAGAEOSAMUNULLNULLJAP2AO2STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24HXDY
CYG OB2 ASSOCIATION308.217541.293580.164910270.83267098220.394954452.918553240754453.84391203740203001041114.74000041114.741114.7041114.7220210037918.137918.179943.90PROCESSED57540.90065972225482854460.65216435183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020150Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku.GALACTIC POINT SOURCES4CKITAMOTOSHUNJINULLNULLJAP2AO2STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130XISY
TEVJ2032+4130308.046141.501680.256131641.05964615221.083954451.98421296354452.917615740740203101040043.94000040043.940043.9040043.9220210037309.137309.180641.91PROCESSED57540.88656255482854460.65696759263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22020150Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku.GALACTIC POINT SOURCES4CKITAMOTOSHUNJINULLNULLJAP2AO2STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130XISY
EV LAC341.712744.3232100.60502245-13.08073089256.160154432.969201388954434.465520833340203201068949.310000068949.369133.3069127.5210210065011.365011.3129232.82PROCESSED57540.79392361115480854441.08768518523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021013We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare.GALACTIC POINT SOURCES4CHWANGUNANULLNULLUSA2AO2FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LACXISY
SIGMA GEM115.84328.9438191.1321433723.30670736104.440354394.409016203754397.9690162037402033010142889.7125000142889.7142993.60142985.62202100124447.1124447.1307541.61PROCESSED57540.40201388895477654407.8304745373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021014Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission on RS CVn binaries. We propose a 125 ksec (3-4 day elapsed time) observation of the RS CVn binary Sigma Gem. Our goals are i) to better characterize its hard (>10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data, and iv) compare long duration flares on Sigma Gem with the 6 hour flares of Sigma2 CrB. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability at 10-25 keV provided by HXD.GALACTIC POINT SOURCES4CBROWNALEXANDERNULLNULLUSA2AO2SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL STRUCTURE ON THE RS CVN BINARY SIGMA GEM (K0III +?)HXDY
HD4322.307259.1394117.5327944-3.28915956247.718154469.703831018554470.515451388940203401038240.64000038248.638240.6038248.6220210035050.335050.3701201PROCESSED57540.99115740745490854483.46355324073.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021016Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior.GALACTIC POINT SOURCES4CAYRESTHOMASNULLNULLUSA2AO2ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTSXISY
HD4322.307959.1397117.53319828-3.2889222246.053554471.695694444454472.29734953740203402026984.42700026984.426984.4026984.41101100246012460151975.90PROCESSED57541.28239583335487154483.38637731483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021016Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior.GALACTIC POINT SOURCES4CAYRESTHOMASNULLNULLUSA2AO2ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTSXISY
ZETA OPH249.2878-10.56286.2837892723.5918074794.945254540.875891203754543.8543287037402038010105583.7100000105591.7105591.70105583.7220210079981.379981.3257317.82PROCESSED57541.95927083335492254553.37853009263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021022Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability.GALACTIC POINT SOURCES4CWALDRONWAYNENULLNULLUSA2AO2MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPHXISY
ETA CARINAE161.2181-59.7282287.59637986-0.67920855289.000654274.245925925954275.901550925940203901058396.15000058404.158396.1058404.122021005155251552143009.91PROCESSED57539.03689814825469554322.51408564823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021026XMM-Newton observations in 2003 suggest that X-ray emission from Eta Carinae has a hard X-ray component above 10 keV in addition to the thermal emission with kT ~3-5 keV. The excess is apparently strongest near the 2-10 keV X-ray maximum, and possibly produced by very hot plasma or 1st-order Fermi acceleration of particles which then inverse Compton-upscatter UV seed photons from the stellar photospheres. We propose a 50 ksec observation of Eta Carinae with the Suzaku telescope during AO2, compare the X-ray spectrum with earlier observations and determine the level of emission at E >9 keV.GALACTIC POINT SOURCES4BHAMAGUCHIKENJINULLNULLUSA2AO2HARD X-RAY EMISSION FROM ETA CARINAEHXDY
RT CRU188.7055-64.6161301.15157727-1.80180428281.60954283.527002314854284.243333333340204001050880.65000050880.650880.6050880.6220210042850.642850.661887.90PROCESSED57539.07443287045469554328.46680555563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021102Symbiotic stars are interacting binaries in which a white dwarf (WD) accretes from the wind of a red giant. Their X-ray emission is typically very soft. Recently, however, 4 symbiotics have been detected out to almost 100 keV. Suzaku observations of two of these sources revealed that the hard X-rays emanated from an extremely hot thermal plasma. One means of producing such hot gas is accretion onto a near Chandrasekhar-mass WD. We propose to use the unique capabilities of Suzaku to test this hypothesis. We will use broad-band X-ray spectral fitting to determine the temperature of the hot plasma, hard X-ray timing studies to search for or constrain rapid variations due to either magnetic or non-magnetic accretion, and Fe line diagnostics to investigate the role of scattering.GALACTIC POINT SOURCES4BSOKOLOSKIJENNIFERNULLNULLUSA2AO2ARE HARD X-RAY SYMBIOTICS PROGENITORS OF TYPE IA SUPERNOVAE?HXDY
VY AQR318.0426-8.830741.59091784-35.22055705252.665254414.652858796354415.385578703740204301025447.32000025447.325447.3025447.3220210022360.522360.563299.92PROCESSED57540.4767129635479054423.17023148153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021105Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA2AO2BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLEXISY
SW UMA129.176953.4845164.8059372236.9600276498.271654410.236770833354410.625219907440204401016899.12000016907.116899.1016907.1110110013896.913896.933551.91PROCESSED57540.43881944445478454417.26975694443.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021105Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA2AO2BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLEXISY
SS AUR93.342347.7333166.012779513.79596984289.108954529.750879629654530.18077546340204501019471.42000019471.419471.4019471.41101100173781737837135.90PROCESSED57541.76990740745490554539.22237268523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021105Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA2AO2BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLEXISY
BZ UMA133.424357.801159.0167276838.83001001307.476754549.992638888954550.444606481540204601029746.62000029754.629754.6029746.6220210024921.224921.239045.90PROCESSED57541.96221064825493354566.22252314823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021105Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA2AO2BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLEXISY
GX17+2274.0087-14.100616.376941941.24456043269.711354362.277303240754362.854340277840205001019095.92000019095.919104.4019095.9210210016044.516044.549849.90PROCESSED57540.01364583335475154384.44870370373.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021111Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA2AO2OBSERVING THE SPECTRUM AND HALO OF GX17+2HXDY
GX17+2274.0098-14.099116.378769291.24433559268.377854370.598807870454371.250219907440205002023011.72000023019.723025.8023011.7320310019048.819048.8562760PROCESSED57540.11393518525476954402.35119212963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021111Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA2AO2OBSERVING THE SPECTRUM AND HALO OF GX17+2HXDY
4U1705-44257.2319-44.0961343.32770356-2.34122442265.63754348.611284722254349.014050925940205101013343.61500013343.613343.6013343.611011009370.69370.634791.91PROCESSED57539.94534722225477354356.26274305563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021113We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARSXISY
4U1705-44257.2347-44.0965343.32858118-2.34307771294.834154381.76327546354382.201550925940205102021971.31500021979.321981021971.311011001568815688378561PROCESSED57540.1981255477054402.65862268523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021113We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARSXISY
4U1705-44257.2244-44.1021343.31966899-2.3404742386.992454516.984756944454517.618217592640205103025995.61500026051.625995.6026051.6220210020820.520820.554723.91PROCESSED57541.71486111115490154535.20304398153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021113We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARSXISY
4U1705-44257.2229-44.1035343.31790137-2.34044351107.415754543.861053240754544.521053240740205104020074.41500020074.420074.4020082.4210210013411.313411.357017.91PROCESSED57541.8995254635492254553.19122685183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021113We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARSXISY
AQL X-1287.8160.578435.71219982-4.14539755284.092554371.649340277854372.06266203740205301013825.21500013825.213825.2013825.221021001374513745357040PROCESSED57540.13271990745476954402.35415509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
AQL X-1287.81790.578935.71351779-4.14685757277.977754376.992777777854377.351608796340205302015132.61500015140.615142.3015132.6110110011890.811890.830999.91PROCESSED57540.14902777785477154403.91571759263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
AQL X-1287.81820.579135.71383379-4.14703266264.958954382.211238425954382.687789351840205303019711.71500019719.719727.7019711.7220210017552.217552.2411620PROCESSED57540.21572916675477054402.57193287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
AQL X-1287.81710.579435.71359616-4.14591745272.602754388.339583333354388.722540205304017915.71500017915.717915.7017915.7220210017668.217668.2330800PROCESSED57540.27528935185476954402.40606481483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
AQL X-1287.81810.577635.7124509-4.14763067265.538454392.383831018554392.791828703740205305017889.91500017889.917889.9017889.9110110016927.816927.835231.91PROCESSED57540.30795138895476954402.41789351853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
AQL X-1287.81720.577535.71194856-4.14687642265.83354397.982407407454398.507222222240205306021364.81500021460.821460.8021364.8220210021402.221402.245343.90PROCESSED57540.33405092595477654407.37472222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
AQL X-1287.82170.579635.71588636-4.14991498243.671554403.274317129654403.6640205307017536.21500017584.217604017536.2110110014332.214332.233319.90PROCESSED57540.37678240745477654409.13201388893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021114We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data.GALACTIC POINT SOURCES4AREMILLARDRONALDNULLNULLUSA2AO2-TOOX-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTSXISY
2S 0921-630140.6632-63.3281.84517925-9.3373938320.563654340.761435185254341.833553240740205701043213.14000043213.143221.1043221.1220210015856.815856.892615.80PROCESSED57539.93049768525472154353.43656253.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220211182S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLUSA2AO2PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630XISY
2S 0921-630140.6643-63.2995281.84516955-9.3366908418.170554342.407916666754343.513472222240205801045693.74000045693.745693.7045693.7220210043346.343346.395499.82PROCESSED57539.90189814825472454356.27607638893.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220211182S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLUSA2AO2PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630XISY
2S 0921-630140.6655-63.298281.84446964-9.335254268.344254335.88702546354336.993217592640205901043131400004313143131043131220210037162.237162.295559.80PROCESSED57539.66618055565472154350.55048611113.0.22.434Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220211182S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLUSA2AO2PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630XISY
2S 0921-630140.666-63.2982281.84477381-9.335234478.34454338.051122685254339.1640206001040342.34000040350.340342.3040350.3110110035646.435646.495799.92PROCESSED57539.67287037045472154350.56293981483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220211182S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum.GALACTIC POINT SOURCES4ACOTTAMJEANNULLNULLUSA2AO2PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630XISY
IGR J17544-2619268.6038-26.33143.23518966-0.3344622484.576554544.526342592654547.2640509259402061010103417.372000103811.5103827.50103417.3220210065565.665565.6236505.93PROCESSED57541.97523148155493354566.61061342593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021121Supergiant Fast X-ray Transients are a newly-discovered class of x-ray binary with short outbursts and late O to early B supergiant companions. They are not persistently bright, but the nature of their low-level variability is not well known. Similarly short outbursts are also seen in bright HMXBs with supergiant companions such as Cyg X-1 and Vel X-1. The mechanism of these outbursts is unknown in all cases. We propose long pointings to the two best-studied SFXTs and a third object, XTE J1743-363, which seems to be transitional between SFXTs and persistent supergiant HMXBs. We will characterize their variability at low flux levels, both to understand the accretion mechanism and to enable surveys of archival data for new SFXTs.GALACTIC POINT SOURCES4CSMITHDAVIDNULLNULLUSA2AO2CHARACTERIZING THE SPECTRUM AND VARIABILITY OF THE SUPERGIANT FAST X-RAY TRANSIENTSXISY
IGR J00370+61229.283661.3722121.21895683-1.451966787.608154273.49984953754274.23077546340206401034908.93000035384.435400.4034908.9220210033792.633792.663141.92PROCESSED57637.52496527785469554322.47142361113.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021122We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities.GALACTIC POINT SOURCES4BTOMSICKJOHNNULLNULLUSA2AO2LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBSXISY
IGR J16207-5129245.1895-51.5038332.45599844-1.0502168788.185554499.823136574154500.7841898148402065010000000000010049595.549595.583031.91PROCESSED57541.4985879635488354515.63478009263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021122We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities.GALACTIC POINT SOURCES4BTOMSICKJOHNNULLNULLUSA2AO2LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBSXISY
IGR J16207-5129245.1891-51.5041332.45561032-1.0502543389.500654526.866111111154527.750219907440206502032612.73000032709.532713.3032612.7220210028331.228331.276375.90PROCESSED57541.74961805565490154535.2085995373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021122We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities.GALACTIC POINT SOURCES4BTOMSICKJOHNNULLNULLUSA2AO2LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBSXISY
IGR J17391-3021264.795-30.3419358.067931220.4485409189.21654518.495011574154519.396122685240206601036465.73000036545.736593.7036465.7220210031259.131259.177819.81PROCESSED57541.71056712965489254525.50646990743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021122We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities.GALACTIC POINT SOURCES4BTOMSICKJOHNNULLNULLUSA2AO2LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBSXISY
4U 1907+09287.40019.896543.798929960.5134463685.383654209.419166666754211.261273148240206701080628.36500080628.380636.3080636.3220210073268.573268.5159147.92PROCESSED57538.45153935185470254216.26741898153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021123The HMXB 4U 1907+09 shows a rich phenomenology: two cyclotron lines, an uncommonly weak iron line, intermittent X-ray fading, and a recent torque reversal. Compared to other persistent supergiant X-ray pulsars it has been less well observed, although it is a prime target to study the interaction of the neutron star's X-rays with the stellar wind and the accretion column. The latter has been confirmed by our 60ks AO1 observation which allowed for the first detection of a soft excess below 2keV as well as the determination of the paramters of the fundamental cyclotron line with unprecedented accuracy. Due to an unusually low source state during the AO1 exposure, however, an additional observation of 65ks is needed to perform the first phase resolved analysis of this interesting source.GALACTIC POINT SOURCES4BPOTTSCHMIDTKATJANULLNULLUSA2AO2THE BROAD BAND SPECTRUM OF 4U 1907+09HXDN
EXO 2030+375308.011837.695177.17399477-1.1745842956.350254234.859166666754236.156527777840206801057607.14000057607.157607.1057607.1220210053395.453395.4112067.82PROCESSED57538.72430555565470254242.4979629633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021124We propose a 40 ks Suzaku observation to confirm EXO 2030+375's recently discovered ~10 keV cyclotron feature and constrain its second harmonic at ~20 keV. EXO 2030+375 is a 42-second Be/X-ray pulsar in an eccentric 46-day orbit. If confirmed the ~10 keV cyclotron feature will be the lowest in energy known for an accreting pulsar and will provide the missing piece to make EXO 2030+375 an ideal candidate to observationally test accretion theory. In addition, we will measure EXO 2030+375's spin frequency, study its pulse shape versus energy, and perform phase resolved spectroscopy. Suzaku will allow these studies to reach lower energies and provide high quality spectra at lower luminosities than in any previous observations.GALACTIC POINT SOURCES4AWILSONCOLLEENNULLNULLUSA2AO2CONSTRAINING CYCLOTRON FEATURES IN A NORMAL OUTBURST OF EXO 2030+375HXDY
4U2206+54331.981154.5897100.6432606-1.0469175590.235754236.162094907454237.812662037402069010103976.8100000103984.8103990.60103976.8330310099784.299784.2142581.91PROCESSED57538.71184027785469554242.766253.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220211254U 2206+54 is a high mass X-ray binary which is suspected to contain a neutron star accreting from the wind of its companion BD +53 2790. However, there has been no confirmed detection of X-ray pulsations, and while several authors have reported hints of a cyclotron line in the energy spectra near 30 keV, none have reported significant detections. We propose Suzaku observations to search for long-period pulsations with the XIS, and possible confirmation of the cyclotron line using HXD/PIN.GALACTIC POINT SOURCES4AFINGERMARKNULLNULLUSA2AO2SUZAKU OBSERVATIONS OF THE PECULIAR HMXB 4U 2206+54HXDY
CIRCINUS X-1230.1633-57.1695322.113849420.03740334115.20654530.195324074154531.552303240740207001046411.34300046411.346411.3046411.3220210041821.341821.31171960PROCESSED57541.80531255491654550.24599537043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021128We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source.GALACTIC POINT SOURCES4ALEEJULIANULLNULLUSA2AO2CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHTXISY
GRS 1915+105288.793310.953545.37037141-0.2113035667.35454227.611365740754229.071747685240207101065656.83700065656.865803.9065672.8120110056897.356897.31261681PROCESSED57538.66409722225470254235.53217592593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021132We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme.GALACTIC POINT SOURCES4AMILLERJONNULLNULLUSA2AO2-TOOTHE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105XISY
CYG X-1299.579235.271971.390341223.1112059384.356554220.816365740754221.78358796340207201045320.43000045320.445328.4045320.4210210040187.340187.3835662PROCESSED57538.5182754635477354228.17185185183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021133We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.GALACTIC POINT SOURCES4ANOWAKMICHAELNULLNULLUSA2AO2CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERAHXDY
CYG X-1299.545135.261871.36718573.1297148559.937154237.820405092654238.648078703740207202033356.83000033356.833364.9033356.8210210032563.732563.771503.91PROCESSED57538.6967245375469554245.01498842593.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021133We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.GALACTIC POINT SOURCES4ANOWAKMICHAELNULLNULLUSA2AO2CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERAHXDY
SWIFT J1753.5-0127268.3714-1.458824.8930086112.1795145261.384654362.858518518554365.437777777840208801094600.59300094608.594616.5094600.5220210081739817392228363PROCESSED57540.11238425935474354371.63663194443.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22021147While the spectrally hard state represents the most common mode of accretion in black hole X-ray binaries, the nature of its accretion flow is poorly understood. We recently discovered cool accretion disks extending close to the innermost stable circular orbit in the hard states of two black hole transients. Such disks could give rise to strong reflection features, but instead these are weak or not detected. We propose a 70 ks Suzaku observation of Swift J1753.5-0127 (one of the two transients), which is currently in a prolonged hard state. Our goal is to put tight constraints on the strength of the reflection features and increase our understanding of the geometry of the spectrally hard component. Understanding accretion onto compact objects is fundamental to NASA's "SEU" theme.GALACTIC POINT SOURCES4AHOMANJEROENNULLNULLUSA2AO2CONSTRAINING REFLECTION FEATURES IN THE HARD STATE OF BLACK HOLE X-RAY BINARIESXISY
TW HYA165.4619-34.7081278.6768548622.9500490399.367354429.061562554429.694606481540208902020009.61100020009.620017.6020025.61101100175501755054687.92PROCESSED57540.59001157415480454434.13872685183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22022007We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra.GALACTIC POINT SOURCES4BSCHMITTJURGENNULLNULLEUR2AO2ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARSXISY
SU AUR73.993430.5715172.51103259-7.9327570785.919754339.171354166754340.750219907440209001057303.45500057311.457303.4057311.4220210054384.854384.8136401.81PROCESSED57539.91146990745472354350.63815972223.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22022007We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra.GALACTIC POINT SOURCES4ASCHMITTJURGENNULLNULLEUR2AO2ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARSXISY
EXO 0748-676117.1051-67.7525279.97237585-19.82332654158.088454459.236956018554460.291944444440209201045898.84000045912.645898.8045904.6220210043574.743574.791135.81PROCESSED57540.97321759265485454483.18393518523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22022014We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity.GALACTIC POINT SOURCES4CDIAZ TRIGOMARIANULLNULLEUR2AO2BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBSXISY
SGR 1806-20272.1687-20.47119.94559743-0.27498509268.139754387.233206018554388.33359953740209401052247.75000052247.752271.7052263.7220210050089.550089.595059.91PROCESSED57540.28395833335477154403.95486111113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22022016Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts.GALACTIC POINT SOURCES4CMEREGHETTISANDRONULLNULLEUR2AO2CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTONHXDY
GT MUS174.8799-65.348295.52044001-3.5163396994.856454446.473668981554449.18766203740209501093308.78000093308.793308.7093308.7220210094696.594696.5234469.93PROCESSED57540.93182870375482854460.77070601853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22022020We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku.GALACTIC POINT SOURCES4BMAGGIOANTONIONULLNULLEUR2AO2BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCEHXDY
HD161103266.1888-27.22721.358501621.05434609105.235154884.794664351854886.705717592640300101071524.96000071532.971524.9071540.9220210059664.759664.7165085.81PROCESSED57545.65332175935533054903.67325231483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030005We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN.GALACTIC POINT SOURCES4BMIURAJUNICHIRONULLNULLJAP3AO3SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUESXISY
HD110432190.599-63.0744301.908501-0.22062002344.942354718.906574074154719.705023148240300201025333.22500025333.225333.2025333.2220210021343.621343.668977.90PROCESSED57543.80376157415514854780.44517361113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030005We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN.GALACTIC POINT SOURCES4BMIURAJUNICHIRONULLNULLJAP3AO3SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUESHXDY
1RXS J070407.9+26250106.031626.4199190.2671404114.2996291596.143754749.126631944454750.368217592640300301053551.95000053551.953551.9053551.9220210041140.541140.5107231.90PROCESSED57544.14569444455514854780.54459490743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030009Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically.GALACTIC POINT SOURCES4BISHIDAMANABUNULLNULLJAP3AO3OBSERVATIONS OF SOFT INTERMEDIATE POLARSXISY
1RXS J062518.2+7334396.330773.5671140.8680157524.12512545262.038354570.038831018554571.125277777840300401050326.75000050326.750326.7050326.7220210050125.350125.393848.80PROCESSED57542.32024305565495354581.23284722223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030009Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically.GALACTIC POINT SOURCES4BISHIDAMANABUNULLNULLJAP3AO3OBSERVATIONS OF SOFT INTERMEDIATE POLARSXISY
1E 1048.1-5937162.5452-59.8394288.24102095-0.47209541101.436854800.959733796354802.5927083333403005010100423.1100000100443100423.10100423.1220210068104.968104.9141081.90PROCESSED57544.60784722225517854812.04718753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030013Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs.GALACTIC POINT SOURCES4CTAKATAJUMPEINULLNULLJAP3AO3X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKUHXDY
MARS-P1102.877325.1625190.2497439411.19384085298.003754559.341481481554559.40994212964030060102904.81000002904.82912.802912.811011002909.62909.65911.90PROCESSED57542.03439814825495354577.04468753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P2102.919825.1641190.2647530811.2294146298.020354559.410092592654559.4932754634030060204854.61000004854.64886.604870.611011003612.13612.17183.90PROCESSED57542.03679398155495354577.03049768523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P3102.961225.1565190.2878403411.26022306298.03254559.493379629654559.57660879634030060303886100000388639100389411011003113.43113.47183.90PROCESSED57542.03731481485495354577.04842592593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P4103.001625.1536190.3061865711.29219101298.047654559.576759259354559.65994212964030060402288.21000002288.22288.202288.21101100201020107183.90PROCESSED57542.04112268525495354577.05289351853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P5103.04525.1496190.3267081411.32616716298.063854559.660046296354559.74324074074030060501956.21000001956.21956.201956.222021001992.61992.67167.90PROCESSED57542.04215277785495354577.13454861113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P6103.084425.143190.3480819911.3557719298.074354559.743437554559.82659722224030060601939100000193919390193911011001804.61804.67181.90PROCESSED57542.04354166675495354577.13763888893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P7103.12725.1401190.3672648411.38956433298.090754559.826747685254559.90298611114030060702502.81000002513.92510.802502.811011001650.61650.665840PROCESSED57542.04883101855495354577.14863425933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P8103.168225.1356190.3873819711.42154102298.106254559.903136574154560.00722222224030060802748.91000002753.82757.802748.922021002286.42286.489840PROCESSED57542.05005787045495354577.16376157413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P9103.219525.1275190.4147374211.46031922298.124754560.007372685254560.07666666674030060902150.61000002150.62174.602150.611011001891.91891.95975.90PROCESSED57542.04888888895495354577.14280092593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P10103.251825.125190.4295485911.48582895298.13554560.076770833354560.164030061003771.61000003795.63771.60379611011004001.44001.47183.90PROCESSED57542.05465277785495354577.15378472223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P11103.293625.1207190.4496979911.5184009298.149354560.160104166754560.24333333334030061104619.81000004627.84619.804635.811011004074.94074.97183.90PROCESSED57542.05594907415495354577.17450231483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P12103.335825.1148190.4714803411.55063865298.164554560.243483796354560.3266666667403006120345510000034553455034551101100267826787175.90PROCESSED57542.05667824075495354577.17894675933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P13103.377925.1101190.4921067611.58330245298.179954560.326770833354560.414030061304251.81000004267.84251.804267.81101100352935297183.90PROCESSED57542.06056712965495354577.92929398153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P14103.418825.1057190.511986511.61511049298.194154560.41015046354560.49333333334030061404825.21000004849.24825.204857.211011003721.43721.47175.90PROCESSED57542.0631255495354577.94347222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P15103.461125.1019190.5318453611.64832678298.208354560.493437554560.57666666674030061503831100000383938310384711011003192.83192.87183.91PROCESSED57542.06222222225495354580.58098379633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P16103.50325.0968190.5527508511.68067717298.222354560.576817129654560.664030061602326.21000002326.22326.202326.22202100213421347179.90PROCESSED57542.06642361115495354577.94789351853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P17103.543925.0908190.574101211.71183533298.23754560.660104166754560.7432870374030061701978.21000001978.21978.201978.211011001959.61959.671820PROCESSED57542.06740740745495354578.04065972223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P18103.586925.0943190.5874376511.74868918298.259254560.743483796354560.82643518524030061801861.81000001861.81861.801861.811011001939.61939.67153.90PROCESSED57542.07055555565495354578.05305555563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P19103.627225.0809190.6154180611.77628093298.267354560.826631944454560.90988425934030061902839.81000002839.82848.202843.822021001844.11844.171900PROCESSED57542.07239583335495354578.04656253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P20103.668525.0732190.6384887911.80707935298.277954560.910034722254560.9932175926403006200184910000018491849018491101100122212227183.90PROCESSED57542.07331018525495354578.05752314823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P21103.710125.0688190.6586060111.8395058298.294754560.993321759354561.07655092594030062102880.81000002880.82880.802880.811011003451.63451.67183.90PROCESSED57542.07748842595495354578.06128472223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P22103.754125.0677190.6765762511.87528798298.311754561.076701388954561.15988425934030062204024.61000004040.64024.604047.61101100410241027183.90PROCESSED57542.07817129635495354578.06656253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P23103.795525.0599190.6997658511.90614711298.32554561.160034722254561.24321759264030062304518.81000004526.84518.804534.811011003686.83686.87183.90PROCESSED57542.07918981485495354578.11761574073.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P24103.838925.0556190.7204680411.94011608298.340154561.243368055654561.3265509259403006240342310000034233423034231101100251125117183.90PROCESSED57542.08443287045495354578.12343753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P25103.880325.0503190.7413253411.97202775298.354654561.326655092654561.40988425934030062504261.21000004269.24261.204269.211011003251.13251.17183.90PROCESSED57542.23364583335495354578.13230324073.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P26103.92125.0474190.7596769112.00436516298.367154561.410034722254561.49321759264030062604797.61000004813.64797.604821.611011003762.23762.27183.90PROCESSED57542.23379629635495354578.13740740743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
MARS-P27103.96425.0399190.7831867812.0366945298.383654561.493321759354561.54181712964030062701099.81000001107.81099.801115.811011001093.51093.54183.90PROCESSED57542.23321759265495354578.12512731483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030015We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase.GALACTIC POINT SOURCES4AEZOEYUICHIRONULLNULLJAP3AO3SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGEXISY
AM HERCULES274.12649.808477.8108207725.81903319234.881454768.859016203754771.3043287037403007010108496.5100000108504.5108504.50108496.5220210094467.194467.1211257.73PROCESSED57544.33924768525515654788.47222222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030021We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object.GALACTIC POINT SOURCES4CTERADAYUKIKATSUNULLNULLJAP3AO3NON THERMAL EMISSION FROM THE POLAR AM HERCULESHXDY
AM HERCULES BGD282.096447.978577.4028541520.2844947234.998654771.307210648254772.343831018540300801044360.14000044368.144360.1044392.1220210040411.540411.589551.91PROCESSED57544.31708333335515454788.42885416673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030021We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object.GALACTIC POINT SOURCES4CTERADAYUKIKATSUNULLNULLJAP3AO3NON THERMAL EMISSION FROM THE POLAR AM HERCULESXISY
ARCHES CLUSTER266.4808-28.7780.169605780.02569084109.999854911.085740740754913.7681712963403009010110793.3100000110793.3110793.30110793.3220210091657.891657.8231741.73PROCESSED57545.95557870375533054924.38221064823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030029We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring.GALACTIC POINT SOURCES4BTSUJIMOTOMASAHIRONULLNULLJAP3AO3A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTERXISY
GX 339-4255.6944-48.7333338.97952784-4.2862048384.726454908.078622685254908.961331018540301101043040.84000043055.443040.8043061.4110110035391.435391.476257.91PROCESSED57545.87364583335533054917.43337962963.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030046Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP3AO3-TOOMULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTHXDY
GX 339-4255.7293-48.7348338.99236079-4.30539701107.954454915.343055555654916.271111111140301102039079.24000039116.539079.2039116.5110110034785.234785.280165.80PROCESSED57545.9098495375533054930.16094907413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030046Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP3AO3-TOOMULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTHXDY
GX 339-4255.7297-48.7352338.99220289-4.30584956108.351354920.477395833354921.521643518540301103039638.44000039663.339638.4039663.3220210035068.635068.6901860PROCESSED57545.97956018525533054931.06104166673.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030046Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP3AO3-TOOMULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTHXDY
LS I+61 303_140.145561.188135.698103741.0510579270.000354853.951585648254854.864803240740301501040551.44000040551.440551.4040551.4220210025731.225731.2788680PROCESSED57545.30229166675532954880.53438657413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030077We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.GALACTIC POINT SOURCES4AFUKAZAWAYASUSHINULLNULLJAP3AO3X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303HXDY
LS I+61 303_240.145761.1877135.698314191.05082335270.000654856.696608796354858.176666666740301601061066.76000061078.461066.7061078.4220210026659.126659.1127839.81PROCESSED57545.38288194445532954880.55221064823.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030077We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.GALACTIC POINT SOURCES4AFUKAZAWAYASUSHINULLNULLJAP3AO3X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303HXDY
LS I+61 303_340.201861.1949135.720052861.06843757246.275354872.184259259354873.725219907440301701068627.36000068627.368627.3068627.3220210065068.565068.5133121.81PROCESSED57545.52908564825533054893.42103009263.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030077We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST.GALACTIC POINT SOURCES4AFUKAZAWAYASUSHINULLNULLJAP3AO3X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303HXDY
HESS J0632+05798.24565.8062205.66072349-1.43796588289.817354579.685682870454580.687719907440301801044076400004407644076044076220210041475.841475.886565.80PROCESSED57542.37466435185496154594.15969907413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030080We propose a 40 ks observation on HESS J0632+057, the newly discovered TeV gamma-ray source in the interacting region of Monoceros SNR and Rosette Nebula. Although this point-like source is found inside the error circle of an unidentified EGRET source 3EG J0634+0521, it has no clear counterpart at other wavelengths. Two sources, a weak X-ray source 1RXS J063258.3+05487 and a Be-star MCW 148, are found inside the error circle of HESS. The aim of the Suzaku observation is to obtain a clue to solve the yet feasible three scenarios of the TeV gamma-ray source.GALACTIC POINT SOURCES4AKOKUBUNMOTOHIDENULLNULLJAP3AO3INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGIONXISY
LMC X -384.7048-64.0785273.57060216-32.09537201185.506754822.301585648254823.867569444440302001073973.86000073973.873981.8073987.5220210070050.570050.5135283.81PROCESSED57545.03478009265520654840.50133101853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030102Ionized iron K absorption lines are commonly observed from high state black hole binaries. Thus the highly ionized plasma are thought to be generally associated with optically thick accretion disks. Huge outflow by the plasma has been confirmed by some of these objects, and thus such plasma is thought to have an important role on accretion flow. In order to establish generality of the plasma by detecting the absorption lines, and to distinguish whether creation mechanism of the plasma is determined by X-ray luminosity or there is another key parameter, we propose Suzaku observation of luminous persistent black hole binary LMC X-3, with exposure of 60ks. This observation will enable us to find critical parameters which determine the creation of the accretion disk wind.GALACTIC POINT SOURCES4CKUBOTAAYANULLNULLJAP3AO3SEARCH FOR IRON K ABSORPTION LINES FROM LMC X-3XISY
RX J1712.6-2414258.1492-24.2444359.86643058.7421524694.458654889.487592592654892.2710532407403021010110481.3100000110489.3110481.30110489.3220210089458.489458.4240441.84PROCESSED57545.75035879635533054908.55883101853.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030106We propose to observe a peculiar Intermediate Polar, RX J1712.6-2414, which has no accretion disk around the white dwarf. This source shows the X-ray modulation only at the beat period and broad Fe-K emission lines in the phase-averaged spectrum. Our goal is to obtain a clear picture about the accretion flow geometry, which can explain the timing and spectral properties, utilizing the fine phase-resolved spectra. Furthermore, we examine the non-thermal emission from the source, since the magnetized white dwarf is a promising candidate of particle acceleration sites.GALACTIC POINT SOURCES4BMORIHIDEYUKINULLNULLJAP3AO3ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414XISY
YY DRA175.868671.6187130.3571290244.51671754282.067654632.775821759354633.409884259340302201029185.13000029185.129185.1029185.1220210027474.327474.354777.91PROCESSED57542.82405092595501354644.15175925933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030107We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4CYUASATAKAYUKINULLNULLJAP3AO3SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
TV COL82.3326-32.8641236.83580562-30.63495041295.914654573.755555555654574.666863425940302301035836.74000035836.735836.7035836.7220210030102.330102.378729.90PROCESSED57542.33930555565495354587.06665509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030107We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4CYUASATAKAYUKINULLNULLJAP3AO3SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
IGR J16194-2810244.8908-28.0663349.166985615.5822360495.187954867.176215277854868.431423611140302401045568.75000045568.745573.8045568.7220210038785.938785.9108435.81PROCESSED57545.48950231485532954880.57435185183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030121We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source.GALACTIC POINT SOURCES4CNAGAEOSAMUNULLNULLJAP3AO3ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810HXDY
V709 CAS7.195159.3013120.03837674-3.4430947984.081654637.433483796354638.154282407440302501035898.23000035898.235898.2035898.2220210033382.333382.362267.90PROCESSED57542.88119212965501454648.33581018523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030140Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP3AO3IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRALXISY
IGR J17303-0601262.5864-5.981417.9378862315.02149808100.792254878.423321759354879.335578703740302601032963.53000032963.532963.5032963.5220210027755.927755.9788182PROCESSED57545.57469907415532554893.43810185183.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030140Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP3AO3IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRALXISY
RX J1940.1-1025295.0445-10.419328.98688715-15.4986964579.740554572.897997685254573.74327546340302701032453.63000032453.632453.6032453.6220210026465.726465.773021.92PROCESSED57542.32410879635495354587.04814814823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030140Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP3AO3IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRALXISY
IGR J17195-4100259.8947-41.0152346.97641748-2.1340075697.063154880.460717592654881.310648148240302801031645.63000031645.631645.6031645.6220210026917.826917.8734280PROCESSED57545.58689814825533054895.54943287043.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030140Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP3AO3IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRALXISY
XSS J12270-4859187.002-48.8936298.9701789813.79783482315.979254686.967442129654687.648078703740302901029623.23000029623.229623.2029623.22202100345803458058791.90PROCESSED57543.20699074075507354707.17302083333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030140Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP3AO3IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRALXISY
WR140305.215943.844680.962576684.11237193190.182554844.541516203754846.50016203740303001089406.88000089406.889406.8089406.8220210078055.778055.7169196.91PROCESSED57545.26096064825532854861.85501157413.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030157WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP3AO3X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140HXDY
WR140305.21143.831880.949985164.10805919199.737154835.358344907454836.425219907440303101047266.44000047266.447266.4047282.42202100453034530392161.80PROCESSED57545.10369212965532854850.21645833333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030157WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP3AO3X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140HXDY
WR140305.194243.80980.924257414.10518752220.540854812.436006944454813.552314814840303201052910.64000052910.652910.6052910.6330310048260.948260.996431.80PROCESSED57544.96128472225519254826.24813657413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030157WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP3AO3X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140HXDY
WR140305.113543.927280.989193944.2199114190.294554565.23140046354565.722430555640303301021625.32000021625.321625.3021625.3220210018605.518605.542415.92PROCESSED57542.26568287045495354580.41856481483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22030157WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP3AO3X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140HXDY
TAU SCO248.9714-28.2185351.5332803112.80600635277.974854710.043668981554710.369722222240303401014617.11000014617.114617.1014617.1110110012085.512085.528135.90PROCESSED57543.44277777785514854780.41701388893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031121We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA3AO3X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCOXISY
TAU SCO248.9731-28.2173351.5352152812.80565459288.702854717.075011574154717.375277777840303402014521.51000014529.514521.5014537.511011009652.49652.425935.91PROCESSED57543.77846064825514854780.61181712963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031121We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA3AO3X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCOXISY
TAU SCO248.9736-28.2151351.5372195512.80675658279.371254723.420729166754723.811967592640303403012290.21000012298.212298.2012290.2110110011028.211028.233799.90PROCESSED57543.81335648155514854780.46315972223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031121We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA3AO3X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCOXISY
TAU SCO248.9733-28.218351.5347893412.80506422280.031254729.417939814854729.757800925940303404013971.11000013971.113971.1013971.1220210012891.212891.2293500PROCESSED57543.8579745375514854780.49540509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031121We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA3AO3X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCOXISY
TAU SCO248.9722-28.2177351.5343737112.80599439271.518154696.314583333354696.667581018540303405016313.61000016350.416313.6016358.411011001396713967304720PROCESSED57543.32256944445508454713.19241898153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031121We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA3AO3X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCOXISY
TAU SCO248.9729-28.218351.5345534412.80533126274.260854703.198159722254703.544722222240303406015018.31000015026.315034.3015018.3110110012904.912904.929911.90PROCESSED57543.38418981485508454713.27549768523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031121We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars.GALACTIC POINT SOURCES4AIGNACERICHARDNULLNULLUSA3AO3X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCOXISY
ETA CARINAE161.2297-59.7314287.60304523-0.6793086529454627.077554627.64952546340303501035447.93000035463.935447.9035463.9220210027210.227210.249415.91PROCESSED57542.76288194455500354637.26800925933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031124X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009).GALACTIC POINT SOURCES4AHAMAGUCHIKENJINULLNULLUSA3AO3X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUMHXDY
ETA CARINAE161.2769-59.635287.57915278-0.5829248399.902754810.2112554811.208495370440303601048501.63000048501.648501.6048501.6220210042425.942425.986151.82PROCESSED57544.68531255519854828.36409722223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031124X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009).GALACTIC POINT SOURCES4AHAMAGUCHIKENJINULLNULLUSA3AO3X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUMHXDY
ETA CARINAE161.3407-59.6518287.61551185-0.58277566142.000654856.133229166754856.682106481540303701028805.33000028805.328805.3028805.3110110017453.917453.947407.90PROCESSED57545.32351851855532854880.5335879633.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031124X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009).GALACTIC POINT SOURCES4AHAMAGUCHIKENJINULLNULLUSA3AO3X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUMHXDY
ETA CARINAE161.3639-59.6742287.63630523-0.59715454170.622854877.52828703754878.411967592640303801035552.53000035568.535552.5035560.5220210031119.331119.376323.91PROCESSED57545.55648148155532854893.43074074073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031124X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009).GALACTIC POINT SOURCES4AHAMAGUCHIKENJINULLNULLUSA3AO3X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUMHXDY
ASAS J002511+1217.26.299712.2847112.91544003-50.07604687234.915654841.681377314854842.54680555564030390103325630000332563325603325622021002987329873747521PROCESSED57545.13487268525532854851.41430555563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031144Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA3AO3BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3XISY
KT PER24.293350.9468130.24865907-11.27406186260.900154843.895706018554844.533495370440304101029195.72000029195.729195.7029195.7220210028165.828165.855089.90PROCESSED57545.16495370375532854854.05479166673.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031144Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA3AO3BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3XISY
SS73 17152.7399-57.7545282.81739372-1.2914309480.155254775.687743055654776.307245370440304301024907200002490724907024907220210020809.120809.153519.90PROCESSED57544.36292824075515754791.63628472223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031145SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission.GALACTIC POINT SOURCES4ASMITHRANDALLNULLNULLUSA3AO3SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17HXDY
GX 301-2186.5611-62.8021300.05773343-0.07103063326.71254703.552280092654704.003668981540304401011427.56000011429.211430.6011427.5220210010714.810714.838993.90PROCESSED57543.39775462965521854720.4354629633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031152We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase.GALACTIC POINT SOURCES4AROTHSCHILDRICHARDNULLNULLUSA3AO3BROAD-BAND STUDY OF GX 301-2HXDY
GX 301-2186.689-62.7212300.108179360.01514837109.009854836.439629629654838.041932870440304402061813.65000061813.661813.6061813.6220210054992.254992.2138398.12PROCESSED57545.13710648155532854851.43031253.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031152We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase.GALACTIC POINT SOURCES4AROTHSCHILDRICHARDNULLNULLUSA3AO3BROAD-BAND STUDY OF GX 301-2HXDY
VELA X-1135.5377-40.5514263.060393393.93722667314.544154634.198113425954635.9043287037403045010104709.6100000104723.4104709.60104715.4220210096008.996008.9147389.91PROCESSED57542.88593755501054644.46878472223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031153We propose to observe the well-known X-ray pulsar Vela X-1 (4U0900-40) using Suzaku in order to test models for the circumstellar environment by measuring teh spectrum and searching for variability in the iron line. The line is expected to exhibit changes in intensity and centroid energy as the X-ray beam sweeps around the wind an illuminates material with varying column density, ionization state, and vleocity. In addition we will study the variability in the cyclotron feature. We will compare our observations with detailed hydrodynamical simulations of the stellar wind and its interaction with the compact object.GALACTIC POINT SOURCES4AKALLMANTIMOTHYNULLNULLUSA3AO3SPECTROSCOPY OF VELA X-1 (4U0900-40) AND SEARCHES FOR PULSE PHASE VARIABILITYXISY
CENTAURUS X-3170.3244-60.5721292.078022410.3860320997.352154808.288611111154810.208553240740304601097587.19000097587.197587.1097587.1220210079656.279656.2165853.70PROCESSED57544.70368055565518854822.62436342593.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031154We ask for a 90 ks observation (which will be performed within typically 180 ks taking Suzaku's duty cycle into account) of the accreting HMXB Centaurus X-3 to conduct the most sensitive study to date of the wide range of changes of its broad band spectrum over one 2.1 binary orbit and with pulse phase. Especially we will determine the evolution of the hydrogen absorption column over the orbit and test whether signatures of the tidal wake observed with RXTE can be confirmed. The variable Fe line complex will be studied. The cyclotron resonance scattering feature of Cen X-3 at ~30 keV is especially well suited to test new physical models describing phase-resolved line profiles, since it is very variable over the pulse, with the line centroid spanning an energy range from 28 to 39 keV.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA3AO3THE BROAD BAND SPECTRUM OF CEN X-3 OVER ORBIT AND PULSE PHASEHXDY
1A1118-61170.3073-61.878292.515895-0.84430143131.712754846.514432870454847.902997685240304901049667.44500049667.449667.4049667.4220210046815.946815.9119953.80PROCESSED57545.23462962965532854858.66031253.0.22.435Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031155We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA3AO3-TOOSEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKUHXDY
1A1118-61170.3215-61.8847292.5244731-0.84831529142.60654859.234432870454859.892581018540305001044212.54500044212.544212.5044212.5220210030915.430915.456859.90PROCESSED57545.36336805565532854880.53262731483.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031155We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA3AO3-TOOSEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKUHXDY
CEN X-4224.5893-31.6684332.2409766823.88258751104.623354847.910231481554850.9717939815403057010146670.4150000146687.6146670.40146691.62202100133618.5133618.5264453.92PROCESSED57545.33545138895532854880.54600694443.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031161Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku.GALACTIC POINT SOURCES4ACACKETTEDWARDNULLNULLUSA3AO3UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4XISY
GX 340+0251.4463-45.6133339.58535361-0.0795348381.2154892.276574074154894.8168287037403060010107312.7100000107314.5107312.70107314.522021008610486104219446.71PROCESSED57545.79135416675532954908.72930555563.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031164In this proposal we request to observe accreting neutron stars sources GX 340+0, GX 3+1 and GX 13+1. The observational goal of the observations is to collect high-spectral resolution data in the region of K$_alpha$ iron line. Our scientific motivation is to put the origin of the line emission under additional theoretical scrutiny. We wish to compare the performance of the wind-reprocessing model to relativistic model in as many sources as possible. This proposal is a part of our broader effort to investigate the origin of iron emission line in Galactic X-ray binaries, which includes a parallel proposal to observe WD binaries.GALACTIC POINT SOURCES4BSHAPOSHNIKOVNIKOLAINULLNULLUSA3AO3IRON KALPHA EMISSION LINE DIAGNOSTICS IN ACCRETING NEUTRON STARSXISY
CYG X-2326.160938.329387.3271497-11.3049575251.120354648.066909722254650.615439814840306301072430.8100000102692.272430.8089814.4110210088133.188133.1220167.80PROCESSED57527.06413194445503154665.31706018523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031165The nature of ultra-dense matter in neutron stars remains enigmatic. To probe this requires accurate neutron star radii and masses. We recently showed that broad iron lines in neutron star low-mass X-ray binaries (LMXBs) constrain the neutron star radius. LMXBs also provide us with another tool, kHz quasi-periodic oscillations (QPOs). Combining the inner disk velocity (from modeling the iron line) and the frequency of the kHz QPOs gives a method to measure the neutron star mass. We propose a 100 ks observation of Cyg X-2 with Suzaku to provide a detailed iron line profile. Combined with simultaneous observations with RXTE to determine the kHz QPO frequency, we will measure the neutron star mass. Cyg X-2 is the perfect test case as it already has a known mass from optical observations.GALACTIC POINT SOURCES4BCACKETTEDWARDNULLNULLUSA3AO3MEASURING NEUTRON STAR MASSES USING BROAD IRON LINES AND KHZ QPOSXISY
CYG X-1299.579735.271471.390126733.1105970384.456554574.681689814854575.423842592640306501033943.53000033943.533978.2033970.3110210028955.628955.6641180PROCESSED57542.37252314825495754587.21174768523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031172We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history.GALACTIC POINT SOURCES4ANOWAKMICHAELNULLNULLUSA3AO3CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERAHXDY
GX 339-4255.7095-48.7885338.94163546-4.32765826281.800954733.94265046354736.096805555640306701010499410000010501810499401049942202100114775.9114775.9186091.72PROCESSED57544.05050925935514854780.58039351853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22031174Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with our multi-wavelength, radio to X-ray, program, Suzaku observations can constrain theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions.GALACTIC POINT SOURCES4ATOMSICKJOHNNULLNULLUSA3AO3-TOOCONSTRAINING MODELS FOR BLACK HOLE ACCRETION IN THE HARD STATEXISY
XTE J1759-220269.9393-22.01187.58310030.7785846986.47954566.518877314854567.646053240740307201048961500004936149425048961220210043912.943912.997363.91PROCESSED57542.29839120375495354580.47665509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22032012Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general.GALACTIC POINT SOURCES4BBOIRINLAURENCENULLNULLEUR3AO3NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHERXISY
V2129 OPH246.9149-24.3651353.2907854216.7250648688.334254866.020243055654866.582129629640307401021033.52000021033.521033.5021033.5220210016533.116533.148533.90PROCESSED57545.44708333335532954880.53177083333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22032022We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties.GALACTIC POINT SOURCES4BROBRADEJANNULLNULLEUR3AO3ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARSXISY
ESO 137-G034248.7664-58.1298329.07669192-7.11373135296.129354744.46265046354746.674583333340307501092052.59000092061.392058.7092052.5220210083661.583661.5191089.71PROCESSED57544.0957754635514854780.60318287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22032025Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas.GALACTIC POINT SOURCES4BGILLIROBERTONULLNULLEUR3AO3ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNERHXDY
GK PER52.820243.8404151.00566373-10.1477205257.514454875.441527777854876.089988425940308101030388.83000030388.830388.8030388.8220210027399.927399.955997.92PROCESSED57545.52606481485533054893.42574074073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22033107We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4CYUASATAKAYUKIHARRISONTHOMASJUS3AO3SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
AE AQUARII310.0451-0.934645.22328928-24.45613885265.162255120.761851851855124.2265393518404001010160454.6160000161451.9161720.90160454.62202100136071.5136071.5299327.73PROCESSED57548.99489583335550355134.55881944443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040032As picked up in the NASA press release in 2008, one of the most important results with Suzaku in three years was the first discovery of a possible non-thermal pulsation from a white dwarf AE Aquarii. This job was performed by our group. "Can magnetized white dwarfs accelerate particles like neutron stars?" This is the basic question of this study as a long standing mystery of Cosmic-ray origin for near 100 years. To ensure our result with Suzaku, we triggered the guest observation of AE Aquarii in TeV gamma-ray band with the recent powerful telescope, H.E.S.S., in their first GO program on 2009. Here, we propose the simultaneous observation with Suzaku and H.E.S.S, to distinguish the acceleration site in and/or outer of the binary system using X-ray and TeV gamma-ray flux informations.GALACTIC POINT SOURCES4ATERADAYUKIKATSUNULLNULLJAP4AO4SUZAKU, H.E.S.S., OPTICAL SIMULTANEOUS OBSERVATION OF THE WHITE DWARF PULSAR, AE AQUARIIHXDY
GS 1826-238277.3735-23.85729.22092987-6.12003001267.286255125.848831018555127.9502777778404007010102515.4100000102515.4102531.40102537.2220210087999.687999.6181541.82PROCESSED57549.01049768525553455166.42208333333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040035We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations.GALACTIC POINT SOURCES4BYAMAOKAKAZUTAKANULLNULLJAP4AO4SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238HXDY
UX ARIETIS51.646628.6421159.59610539-22.97107378272.696655229.711666666755231.732106481540400801087799.39000087799.387799.3087799.3220210079742.979742.9174539.90PROCESSED57550.51662037045561655249.8301504633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040036We propose a hard X-ray observation of RS CVn-type active binary UX Arietis. Detection of nonthermal hard X-ray radiation is essentially important to solve the generation mechanism of stellar flares. UX Ari has a high coronal activity with a high temperature of ~2keV, and large stellar flares were frequently observed in the radio, UV, and X-ray band. Therefore, UX Ari is very suitable for hard X-ray observation of stellar flares. Large X-ray flares were observed by BeppoSAX, ASCA and Ginga sattellite, and hard X-ray emission upto ~50keV is detected by BeppoSAX. If a flare is large such as the events of former X-ray observations, we can detect the nonthermal hard X-ray emssion by Suzaku HXD.GALACTIC POINT SOURCES4CISHIKAWASHIN-NOSUKENULLNULLJAP4AO4STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETISHXDY
RXJ0007.0+73021.891672.9843119.6870038210.38954096241.732855204.611284722255207.0675231482404011010105373.9100000105373.9105373.90106971.4220110058564.458564.4212205.92PROCESSED57550.19585648155558755768.96333333333.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040054We propose to observe the gamma-ray pulsar and itswind nebula (PWN) in the supernova remnant CTA1 with SUZAKU. Observations in X-ray wavebands are crucial to study non-thermal processes of PWNe. Its flux and spectral shape provide us important information about the energy distribution of the accelerated particles and the strength of the magnetic field. Observations made by Suzaku-HXD will constrain the X-ray spectrum above 20keV from the PWN for the first time. The high spectral resolution of XIS will allow us to search for metal lines, which tell us circumstance of the emission region. In addition, we will probably able to detect X-ray pulsation, which has notbeen detected yet, using XIS timing mode.GALACTIC POINT SOURCES4CTAKATAJUMPEINULLNULLJAP4AO4X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1HXDN
U SCO245.6288-17.8156357.7207961321.9090119493.274755233.010243055655234.291886574140401801046076.42000046076.446076.4046076.4220210037611.737611.7110719.91PROCESSED57550.5185995375561755250.15593753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040057We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.GALACTIC POINT SOURCES4ATAKEIDAINULLNULLJAP4AO4-TOOTOO OBSERVATION OF A RECURRENT NOVA EXPLOSIONHXDY
U SCO245.629-17.8143357.7219988121.9097056393.27455236.51437555237.166886574140401802028936.92000028936.928936.9028936.9220210018328.818328.856369.90PROCESSED57550.55653935185561955251.14986111113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040057We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.GALACTIC POINT SOURCES4ATAKEIDAINULLNULLJAP4AO4-TOOTOO OBSERVATION OF A RECURRENT NOVA EXPLOSIONHXDY
U SCO245.6292-17.8133357.7229545321.9102056793.275355239.29922453755239.825902777840401803026826200002682626826026826110110024903.724903.7454721PROCESSED57550.56107638895561955253.11556712963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040057We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each.GALACTIC POINT SOURCES4ATAKEIDAINULLNULLJAP4AO4-TOOTOO OBSERVATION OF A RECURRENT NOVA EXPLOSIONHXDY
EUVE J0317-85.548.9864-85.5003299.84736337-30.7288152965.4655028.601747685255030.146018518540401901063084.36000063084.363084.3063084.3220210056896.556896.5133413.81PROCESSED57547.87128472225540655040.26743055563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040083Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects.GALACTIC POINT SOURCES4BHARAYAMAATSUSHINULLNULLJAP4AO4FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARFHXDY
V603 AQL282.22460.597633.174318220.8375150193.952955267.015659722255267.977303240740402001034917.33000034930.934917.3034930.9220210030204.530204.583077.81PROCESSED57550.86560185185564555279.44712962963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040095The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP4AO4IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLESXISY
TT ARI31.718115.2972148.52228749-43.7944371.066855018.442465277855019.302361111140402101035742.13500035742.135779.6035787.62202100317943179474257.81PROCESSED57547.78224537045539955029.2367129633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040095The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP4AO4IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLESXISY
Z CAM126.299373.0997141.3955017932.62975748289.099854931.118715277854931.909247685240402201037663350003766337663037663220210036532.936532.968289.90PROCESSED57546.11597222225532454949.45178240743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040095The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP4AO4IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLESXISY
HESS J0632+05798.24485.8057205.66080027-1.43890266289.963154941.563194444454944.1542708333404027010100034.3100000100034.3100034.30100034.3220210082391.882391.8223841.96PROCESSED57546.24064814825533654966.53239583333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040102We propose a coordinate observation of HESS J0632+057 with Suzaku and VLA. This source is recently discovered as a fourth gamma-ray binary with HESS and XMM-Newton, and our results obtained in Suzaku AO-3 also confirmed a gradual variety of X-ray intensity, possibly associated with the binary period. With a combined observation with VLA, we will for the first time obtain a "real-time" variety from both of image and spectrum of this interesting source.GALACTIC POINT SOURCES4AKOKUBUNMOTOHIDENULLNULLJAP4AO4SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLAXISY
BG CMI112.84889.8847208.5199729613.31865509292.79354932.507870370454933.571053240740402901047079.14000047087.147079.1047087.1110110045034.645034.6918082PROCESSED57546.12239583335532454949.52790509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040113We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4AYUASATAKAYUKINULLNULLJAP4AO4SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
PQ GEM117.796714.685206.1034488719.72488518295.288954933.573703703754934.632916666740403001046738.74000046738.746738.7046738.7220210043247.943247.991507.90PROCESSED57546.14057870375532454949.53179398153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040113We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4AYUASATAKAYUKINULLNULLJAP4AO4SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
TX COL85.7822-41.0648246.79781267-29.77494364322.482754963.680057870454965.250219907440403101059781.84000059789.859789.8059781.8220210051123511231356540PROCESSED57546.57341435185534554978.21054398153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040113We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4AYUASATAKAYUKINULLNULLJAP4AO4SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
FO AQR334.4646-8.293153.06192299-49.1130909876.418654987.343715277854988.553692129640403201046084.64000046084.646084.6046084.6220210033499.333499.3104529.90PROCESSED57547.51533564825536654998.32710648153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040113We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4AYUASATAKAYUKINULLNULLJAP4AO4SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
AO PSC343.7945-3.127168.69841137-53.2857853960.946155004.493414351855005.332858796340403301039654.44000039654.439662.4039662.4220210035683.435683.472517.90PROCESSED57547.63064814825538555018.1654745373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22040113We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space.GALACTIC POINT SOURCES4AYUASATAKAYUKINULLNULLJAP4AO4SURVEY OBSERVATION OF INTERMEDIATE POLARSHXDY
HD690317.450719.662128.84764567-42.998703470.000455031.382430555655032.357870370440403401036813.53500036829.536813.5036821.5220210029672.729672.784263.90PROCESSED57547.88239583335541955048.30299768523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041201Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior.GALACTIC POINT SOURCES4BAYRESTHOMASNULLNULLUSA4AO4ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAPXISY
HD72779128.830819.5933205.5101820931.33811175104.321455141.324594907455142.951527777840403501071033.57000071033.571033.5071033.522021004746147461140555.90PROCESSED57549.21559027785553255166.20741898153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041201Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior.GALACTIC POINT SOURCES4BAYRESTHOMASNULLNULLUSA4AO4ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAPXISY
YY MEN74.6207-75.281287.41045099-33.230691927.258754996.077291666754998.5606365741404036010106949.8100000106957.8106957.80106949.82202100104090.2104090.2214539.80PROCESSED57547.62403935185537855008.29971064823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041202The single K giant YY Men is one of the most active stars within 300 pc of the Sun, having produced 2 of the most powerful radio flares and 1 of the most powerful and long-duration optical flares ever detected. Its corona is one of the hottest and brightest known, with a *typical* X-ray luminosity of 32.0-32.5 (log erg/s) which most other cool stars only reach during major flares. We propose to obtain a 100-ksec observation of this hyperactive star to get a high S/N XIS exposure of its spectrum, particularly in the 5-10 keV region in which the XIS excels. We will study the He- and H-like Fe lines, search for 6.4 keV fluorescent emission, search for the presence of ultrahigh temperature and nonthermal spectral components, and look for correlations with simultaneous ATCA radio observations.GALACTIC POINT SOURCES4BDRAKESTEPHENNULLNULLUSA4AO4THE EXTREME CORONAL PROPERTIES OF THE HYPERACTIVE K GIANT YY MENXISY
V773 TAU63.559128.1916168.22897578-16.34488481264.318355255.966655092655258.750162037404037010115405.7120000115405.7115405.70115405.722021009556395563240466.71PROCESSED57550.84991898155563755271.4995370373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041203Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence.GALACTIC POINT SOURCES4COSTENRACHELNULLNULLUSA4AO4X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAUXISY
ETA CARINAE161.2306-59.7313287.60339978-0.67900846291.999854992.823414351854994.291886574140403801051225.94500051225.951233.9051233.9220210049118.649118.6126839.80PROCESSED57547.56673611115537855006.24475694443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041204The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements.GALACTIC POINT SOURCES4AHAMAGUCHIKENJINULLNULLUSA4AO4HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CARHXDY
ETA CARINAE161.2575-59.6351287.57052339-0.5875858687.891955156.188344907455157.319664351840403901049388.74500049388.749388.7049388.7220210034255.334255.397720.10PROCESSED57549.52871527785554255176.36513888893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041204The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements.GALACTIC POINT SOURCES4AHAMAGUCHIKENJINULLNULLUSA4AO4HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CARHXDY
SKY(270, +25)270.255825.150450.9992040121.6897641770.653855284.562002314855285.29947916674040410101701.9250001926.62094.401701.922021005621.15621.163713.91PROCESSED57551.05402777785528455301.26523148153.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041222Suzaku has recently revealed relativistically broadened Fe Kalpha emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs that we have examined, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Only with the sensitivity of Suzaku, its high effective area in the Fe K band, and its broad bandpass has it been possible to robustly determine the shape of the lines. With a longer-term aim of completing a census of iron lines in neutron star LMXBs, we request a total of 200 ks to observe 5 neutron star low-mass X-ray binaries to study the relativistic broadening in the Fe Kalpha emission line profiles.GALACTIC POINT SOURCES4CCACKETTEDWARDNULLNULLUSA4AO4AN FE KALPHA EMISSION LINE SURVEY OF NEUTRON STAR LMXBSHXDY
4U 1608-52243.1847-52.3651330.96850701-0.8105653396.608555266.07765046355267.007222222240404401034010.13000034010.134010.1034010.12202100301943019480297.80PROCESSED57550.83059027785564755279.45916666673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041223The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona.GALACTIC POINT SOURCES4ACACKETTEDWARDNULLNULLUSA4AO4-TOOACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURSTHXDY
4U 1608-52243.1805-52.3646330.96698106-0.8084441694.031655270.693761574155271.666828703740404402032718.13000032718.132726.1032718.12102100269882698884055.81PROCESSED57550.90652777785565155285.11754629633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041223The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona.GALACTIC POINT SOURCES4ACACKETTEDWARDNULLNULLUSA4AO4-TOOACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURSTHXDY
4U 1608-52243.2309-52.3757330.98178647-0.83761569125.760655273.998668981555274.915416666740404403031756.83000031756.831756.8031756.8220210015309.415309.479193.80PROCESSED57550.91918981485565255286.2598495373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041223The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona.GALACTIC POINT SOURCES4ACACKETTEDWARDNULLNULLUSA4AO4-TOOACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURSTHXDY
4U 1608-52243.1735-52.4241330.92310685-0.84886634127.998355277.98984953755278.914039351840404404016072.83000016072.816072.8016072.8330310015655.715655.779843.92PROCESSED57550.98054398155566555299.41288194443.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041223The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona.GALACTIC POINT SOURCES4ACACKETTEDWARDNULLNULLUSA4AO4-TOOACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURSTHXDY
A 0535+2684.719526.3786181.38803208-2.6160946186.185655067.962627314855069.159942129640405401051866.84500051870.651870.6051866.822021004207842078103429.81PROCESSED57548.36677083335544855078.2198379633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041232We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA4AO4-TOOCYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKUHXDY
A 0535+2684.729126.2457181.50526016-2.67952465272.255555292.502407407455293.70292824074040550103177.9450003177.93460.403177.9220210034392.834392.8103715.81PROCESSED57553.00490740745568955323.44355324073.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041232We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA4AO4-TOOCYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKUHXDY
IGRJ16393-4643249.7688-46.7009338.001775010.07896045111.662755267.986574074155269.450856481540405601050540500005056450540050564220210042256.542256.5126467.81PROCESSED57550.87541666675564755279.46866898153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041234Stellar winds play a critical role in several as yet poorly understood astrophysical processes. One of the best laboratories for studying winds is in wind fed Supergiant High Mass X-ray binaries. Using the neutron star (NS) as a backlight, variable absorption in X-rays measures column density variations in the secondary star wind. A recent explosion in the number of known HMXBs has defined two additional subclasses of HMXBs, potentially related through geometry and wind properties: 1) heavily obscured sources and 2) so-called Supergiant Fast X-ray Transients (SFXTs). We propose observations of 2 obscured sgHMXBs and 2 SFXTs to monitor the column density. This will test wind models and probe whether these subclasses are related to one another and to classical HMXBs through wind parameters.GALACTIC POINT SOURCES4CMORRISDAVIDNULLNULLUSA4AO4PROBING DONOR STAR WIND STRUCTURE IN HMXBS THROUGH VARIABLE ABSORPTIONXISY
GS 2023+338306.044433.801573.0785131-2.14854563252.452155142.963680555655144.055081018540405901042324.64000042348.642324.6042356.6220210029140.429140.494283.91PROCESSED57549.18873842595553155155.10656253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041243The quiescent state is the dominant accretion mode for black holes on all mass scales. Our knowledge of the X-ray spectrum is limited due to the characteristic low luminosity in this state. Here, we propose a 40 ks observation of the most luminous quiescent stellar mass black hole GS 2023+338 (V404 Cyg). These observations will allow us to detect hard X-ray emission from a quiescent stellar mass black hole for the first time, providing unique contraints on the nature of the accretion flow in this low luminosity state.GALACTIC POINT SOURCES4BREYNOLDSMARKNULLNULLUSA4AO4CONSTRAINING THE QUIESCENT ACCRETION FLOW AROUND A BLACK HOLE WITH SUZAKUHXDY
GRS 1758-258270.2971-25.6794.56169204-1.3256306189.381755263.898333333355266.071111111140406001082682.78000082682.782682.7082682.7220210071178.971178.9187709.71PROCESSED57550.86645833335564755279.54684027783.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041244We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state.GALACTIC POINT SOURCES4BREYNOLDSMARKNULLNULLUSA4AO4CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258HXDY
LMC X-184.947-69.7479280.20680376-31.5031657510.000455033.77672453755036.8953587963404061010129867.9120000129867.9129867.90129867.92202100132597.6132597.6269395.64PROCESSED57548.01995370375541955048.65091435183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041245We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability.GALACTIC POINT SOURCES4AMCCLINTOCKJEFFREYNULLNULLUSA4AO4MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINEXISY
LMC X-384.7128-64.0821273.5746003-32.09166858184.452155186.526516203755190.9105555556404062010154424.21500001544341544340154424.22202100101172.1101172.1352145.82PROCESSED57550.13649305565558755218.73843753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22041245We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability.GALACTIC POINT SOURCES4CMCCLINTOCKJEFFREYNULLNULLUSA4AO4MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINEXISY
XTE J1710-281257.5483-28.1282356.358391866.9261344786.227555278.920763888955281.146030092640406801076138.57500076138.576146.5076146.5330310023656.523656.5192239.73PROCESSED57551.04664351855566855301.52276620373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042003We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV.GALACTIC POINT SOURCES4CBOIRINLAURENCENULLNULLEUR4AO4SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPSXISY
4U 1820-30275.9267-30.42342.73525617-7.94773658265.181555083.112002314855083.20157407414040690103517.5200003525.53517.503525.511011003712.43712.477380PROCESSED57548.50525462965547555109.42031253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1820-30275.9248-30.42092.73676025-7.94514519265.931955088.364583333355088.814108796340406902021037.32000021037.321037.3021037.31101100171701717038831.90PROCESSED57548.5698379635546955103.44574074073.0.22.433Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1820-30275.9316-30.42062.73970623-7.95024046261.875555096.044745370455096.833541666740406903029225.42000029225.429225.4029225.4210210025940.525940.5681481PROCESSED57548.65987268525547755110.39896990743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1820-30275.9314-30.41932.74079847-7.94949913261.876255102.669675925955103.500266203740406904028699.42000028699.428699.4028699.4320310024926.124926.171751.92PROCESSED57548.67525462965549955133.22732638893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1820-30275.9251-30.41722.74021083-7.94370371265.200955111.109664351855111.70016203740406905021767.42000021767.421767.4021767.4110110015674.315674.351003.90PROCESSED57548.77998842595549655127.29381944453.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1820-30275.9218-30.42062.73584989-7.94270191269.396455116.632106481555117.175914351840406906024668.7100000024668.7024668.7010210016950.516950.5469780PROCESSED57548.87548611115550755131.36935185183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1820-30275.9205-30.42122.7347979-7.94197311270.416455124.235613425955124.792581018540406907024056.610000024056.724072.6024056.6310210018903.518903.548107.90PROCESSED57548.91939814825550355134.24273148153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042004Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLEUR4AO4ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
IGR J08408-4503130.2449-45.0216264.03123634-1.90203871133.443255176.745219907455179.5002199074404070010925661000009264692566092630220210069434.469434.4237989.82PROCESSED57549.86972222225556755200.39415509263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042007We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class.GALACTIC POINT SOURCES4CSIDOLILARANULLNULLEUR4AO4SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503HXDY
GX 9+9262.9404-16.89298.575056949.0692003497.532955271.673877314855273.991898148240407101085187.17500085208.785203.1085187.1210210061694.261694.2200263.90PROCESSED57550.97674768525565255285.41795138893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22042011We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations.GALACTIC POINT SOURCES4BDIAZ TRIGOMARIANULLNULLEUR4AO4A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONSHXDY
CYGNUS X-1299.596435.272371.398009533.0994280495.812354924.053738425954924.565428240740407501015309.130000015309.115318.8015310.8210210015537.415537.444203.91PROCESSED57546.01134259265492254949.49178240743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.589535.272171.394899283.1041321391.310354929.256284722254929.822442129640407502021336.130000021336.121336.1021336.1210210013125.813125.8489140PROCESSED57546.07826388895492254949.49031253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.589135.27271.394643413.1043587891.311354935.765046296354936.147395833340407503017108.830000017108.817116.8017108.82102100129861298633027.91PROCESSED57546.14526620375492254949.53032407413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.579135.271971.390298633.1112756284.053654944.167476851854944.62527777784040750401801430000018016.618014018016.6110110016327.716327.7395500PROCESSED57546.20940972225492254966.31253.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.581435.271271.390679813.1093080985.143354949.709988425954950.217592592640407505020521.230000020529.220535.4020521.2210210012401.312401.343845.90PROCESSED57546.44754629635492254976.20306712963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.539235.258971.362194213.1323183755.325454957.700682870454958.135636574140407506019434.530000019434.519450.5019434.5210210015279.515279.537557.90PROCESSED57546.51214120375492254976.08853009263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.665335.16571.335704592.99545336212.800455182.061932870455182.550856481540407507022101.930000022101.922109.902366411011003460.73460.7422360PROCESSED57549.87556712965492255200.44900462963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDN
CYGNUS X-1299.543435.259271.364238783.1295464157.797754971.024259259354971.604386574140407508021340.430000021340.421348.4021340.4210210017495.417495.450119.91PROCESSED57546.60888888895492254992.65468753.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.537335.257371.36001723.1328101453.489554976.358206018554976.825972222240407509020925.230000020925.220933.2020925.2210210016116.416116.4404121PROCESSED57546.67962962965492254992.66517361113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.533735.254571.356090353.1338626250.094454980.495671296354981.058622685240407510028784.530000028784.528784.5028784.5110110025738.925738.948631.91PROCESSED57546.72924768525492254994.38728009263.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.529435.251571.351694473.1352993246.767554984.48140046354984.987083333340407511017450.23000001903717778.2017450.2110110015040.915040.943687.91PROCESSED57547.44754629635492254994.40910879633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.527235.249771.349218693.135896544.783454986.820833333354987.335694444440407512016873.330000016881.316889.4016873.321021006764.76764.744477.91PROCESSED57547.48060185185492255001.01630787043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.602135.130871.279498743.02171591263.229955125.377210648255125.840439814840407513020498.530000020498.520506.5020498.52102100151631516340015.90PROCESSED57548.94052083335492255134.27019675933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.608635.131971.283213363.01775246259.206955130.265231481555130.748136574140407514023104.230000023104.223128.2023120.221021002001120011417160PROCESSED57548.99431712965492255141.35394675933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.620635.133971.290045353.01042005252.178855138.894618055655139.410636574140407515022616.830000022616.822624.8022616.82102100140611406144575.91PROCESSED57549.05939814825492255149.42021990743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.627735.137171.295811163.00713364246.543355145.819398148255146.437719907440407516026022.230000026022.226038.2026026.5210210018250.518250.5534160PROCESSED57549.25771990745492255176.20274305563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.635535.139771.301363283.00304649241.225955152.285509259355152.941828703740407517023448.530000023448.523888.5023880.5210210018707.118707.156691.83PROCESSED57549.43565972225492255162.20192129633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.635435.139771.301320583.00311627241.155755159.51422453755160.132858796340407518021768.530000021768.522480.5022472.5520310011406.411406.453435.80PROCESSED57549.57836805565492255176.2948495373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.653735.151871.319473532.99665901225.815955166.292245370455166.890439814840407519022415.530000022415.522431.5022423.5210210013157.813157.851673.90PROCESSED57549.66472222225492255181.2889120373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDY
CYGNUS X-1299.654935.155571.323147132.99775182222.729555173.64734953755174.104328703740407520020016.630000020016.621752.6021859.3110110017442.617442.639471.90PROCESSED57549.72339120375492255189.27524305563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22044131In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals.GALACTIC POINT SOURCES4AMILLERJONYAMADASHINUSJ4AO4A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLEHXDN
1E 2259+586345.271658.9493109.11022544-0.9289550486.323954976.833530092654978.6446064815404076010122579.1120000122580.9122580.90122579.12202100103446.2103446.2156463.81PROCESSED57546.72987268525492254992.69350694443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22046002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP4AO4A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
SGR 1900+14286.79869.387343.073775350.8052618482.670454947.766481481554949.080717592640407701053137.45000053393.453393.4053137.4220210042101.142101.1113547.91PROCESSED57546.46944444445492254973.45472222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22046002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP4AO4A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
SGR 0501+451675.279545.3414161.495681491.9897653893.334155060.848506944555061.834884259340407801042675.34000042675.342955.3042891.3220210027487.827487.885185.80PROCESSED57548.17800925935492255071.25943287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22046002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP4AO4A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
4U0142+6126.517661.8112129.33625727-0.3793359961.04155055.070312555057.3654976852404079010107412.9100000107412.9107420.90107422.7220210099757.699757.6198283.82PROCESSED57548.20121527785492255068.30372685183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22046002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP4AO4A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
1RXS J1708-4009257.2032-40.2034346.44001394-0.00188973266.402155066.684120370455067.946689814840408001060886.96000060886.960894.9060904.6320210051531.351531.3109075.81PROCESSED57548.3501504635492255078.17518518523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22046002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP4AO4A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
PSR J1846-0258281.5972-2.910629.7662115-0.2047410886.000154936.817557870454939.6779398148404081010104345.1100000104345.1104367.50104353.1220210076006.576006.5247101.81PROCESSED57546.27469907415492254959.50060185183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22046002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP4AO4A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
IGR J15094-6649227.3484-66.8278315.91945149-7.5010923390.462655588.703136574155589.555763888940500701049461.25000049483.249475.2049461.2220210048018.548018.573659.90PROCESSED57600.78300925935599055621.22822916673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050025The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system.GALACTIC POINT SOURCES4CYUASATAKAYUKINULLNULLJAP5AO5ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINESXISY
V773TAU63.557128.1952168.22500409-16.34364304260.655755610.158171296355611.981527777840501101082246.38000082254.382246.3082254.3220210072828.772828.7157525.82PROCESSED57601.02561342595599055621.29787037043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050033We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band.GALACTIC POINT SOURCES4BTSUBOIYOHKONULLNULLJAP5AO5NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLAREXISY
PSR J1429-5911217.5051-59.1899315.267808511.30018252101.12455588.226562555588.700115740740501201030382.43000030390.430398.4030382.4110110028792.328792.340903.90PROCESSED57600.75623842595596855602.14045138893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050047Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.GALACTIC POINT SOURCES4CKAWAINOBUYUKINULLNULLJAP5AO5X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARSXISY
PSR J1044-5737161.1338-57.616286.570191061.16750605109.197355542.298425925955542.729293981540501301022630300002263022630022635.8110110021960.321960.3372000PROCESSED57554.37531255591755550.96481481483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050047Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.GALACTIC POINT SOURCES4CKAWAINOBUYUKINULLNULLJAP5AO5X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARSXISY
PSR J0614-3393.5386-33.5015240.50300829-21.83180137119.148455498.971967592655499.614074074140501401031210.93000031210.931210.9031210.9220210027331.427331.455449.90PROCESSED57553.89857638895587555509.03597222223.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050047Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.GALACTIC POINT SOURCES4CKAWAINOBUYUKINULLNULLJAP5AO5X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARSXISY
PSR J2055+2539313.95725.650570.67687842-12.53222207262.322955498.147939814855498.957835648240501501031106.93000031106.931106.9031106.9110110021458.121458.169967.90PROCESSED57553.89675925935589055523.99273148153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050047Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.GALACTIC POINT SOURCES4CKAWAINOBUYUKINULLNULLJAP5AO5X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARSXISY
PSR J1957+5036299.435450.547484.5848016110.99652902216.564955543.458668981555544.084293981540501601032469300003248532469032485220210025313.925313.954033.92PROCESSED57554.39653935185595955592.93417824073.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050047Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars.GALACTIC POINT SOURCES4CKAWAINOBUYUKINULLNULLJAP5AO5X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARSXISY
V2487 OPH262.9946-19.30616.539057627.73892052274.127755478.288043981555479.582789351840502101056307.65000056315.656307.6056323.6220210051358513581118322PROCESSED57553.67718755585455488.1792245373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050059Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141.GALACTIC POINT SOURCES4ATERADAYUKIKATSUNULLNULLJAP5AO5SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKUHXDY
IGR J00234+61415.709261.7549119.55446517-0.9291467480.28655372.00437555373.239756944540502201081880800008188081880081880220210070036.470036.4106697.91PROCESSED57552.43717592595578055414.17916666673.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050059Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141.GALACTIC POINT SOURCES4ATERADAYUKIKATSUNULLNULLJAP5AO5SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKUHXDY
1E 1547.0-5408237.7284-54.3676327.20000551-0.18012949271.166355415.161192129655415.963379629640502401051672.85000051672.851792.8052152.9220110042781.242781.269299.90PROCESSED57552.88709490745579355427.2470254633.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050099Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks.GALACTIC POINT SOURCES4BNISHIOKAHIROYUKINULLNULLJAP5AO5OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATEHXDN
EMS0918211.2948-61.3938311.640553540.22486043106.82255589.558831018555590.083483796340502501024542.52000024550.524542.5024558.5220210023281.123281.145309.91PROCESSED57600.77346064825597255602.20150462963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050104Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.GALACTIC POINT SOURCES4ATANAKAYASUYUKINULLNULLJAP5AO5SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCESXISY
EMS1150263.083-32.7212355.277400660.3930669891.245255611.996493055655612.696805555640502601020918.62000020918.620918.6020918.6110110017263.917263.960503.90PROCESSED57600.97778935185598855621.14407407413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050104Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.GALACTIC POINT SOURCES4ATANAKAYASUYUKINULLNULLJAP5AO5SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCESXISY
EMS01095252.3381-45.0256340.43907916-0.1782734887.553455603.154432870455603.761331018540502701020933.22000020934.420934.4020933.2220210016976.216976.252431.90PROCESSED57600.90930555565598355617.41274305563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050104Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.GALACTIC POINT SOURCES4ATANAKAYASUYUKINULLNULLJAP5AO5SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCESXISY
EMS1308293.039319.256754.622892890.1082733290.000155313.436574074155313.976620370440502801023898.72000023906.723906.7023898.732021002320923209466521PROCESSED57551.3064004635569355327.17899305563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050104Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV.GALACTIC POINT SOURCES4ATANAKAYASUYUKINULLNULLJAP5AO5SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCESXISY
V1280 SCO254.4172-32.3368351.334700396.559698597.745155605.366261574155608.0501851852405029010996831000009969999683099699220210086930.686930.6231873.92PROCESSED57600.99784722225598355617.41423611113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050110We propose a 100 ks observation of the C-rich classical nova V1280 Sco. Using Suzaku's excellent spectral performance in the soft X-ray energy band, we aim to detect and to resolve emission lines from C, N, and O.GALACTIC POINT SOURCES4ATAKEIDAINULLNULLJAP5AO5X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCOXISY
HD125599215.4515-48.0762318.1513784912.10713587289.165355414.676006944455415.157199074140503001031048300003105631056031048110110024859.924859.941567.90PROCESSED57552.86152777785579355427.17538194443.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050116Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP5AO5QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSIONXISY
HD130693222.5749-24.4173334.7129389831.01917553104.633755580.652592592655581.238437540503101021314.52000021314.521314.5021314.5220210017462.517462.550605.92PROCESSED57600.66488425935596555598.98315972223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050116Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP5AO5QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSIONXISY
XSS J16537-1905253.8855-18.14472.5669910515.5263431696.756955602.704641203755603.148865740740503201020024.32000020032.320040.3020024.3220210018152.818152.838343.90PROCESSED57600.8873379635598355617.41042824073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050116Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP5AO5QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSIONXISY
XSS J17223-7301259.6949-73.4263319.10640118-19.70481928106.664355302.15265046355302.593946759340503301033386.13000033386.133386.1033386.1220210025588.925588.938127.90PROCESSED57551.23737268525569255326.14377314823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22050116Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources.GALACTIC POINT SOURCES4BEBISAWAKENNULLNULLJAP5AO5QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSIONXISY
EG AND11.16840.673121.54657283-22.18054863225.211155597.628101851855600.0030092593405034010100533.3100000100533.3100541.30100549.3220210084658.984658.9205171.93PROCESSED57600.92416666675598355614.29721064823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051211The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae.GALACTIC POINT SOURCES4CNELSONTHOMASNULLNULLUSA5AO5EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARSXISY
4 DRA187.484169.1938125.7722908447.81569563339.996955304.891377314855305.855729166740503501042260.24000042268.242268.2042260.22202100437924379283277.81PROCESSED57551.25554398155569355327.21739583333.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051212The symbiotic star, 4 Dra, has been poorly studied in X-rays. Based on the ROSAT data, we argue that it is a nearby, lower accretion rate analogue of the hard X-ray bright symibiotic stars that have been detected above 10 keV. We propose the first pointed observation of 4 Dra that covers the entire 0.4-10 keV band to test our interpretation: we expect it to be bright above 2 keV, with an optically thin thermal spectrum, likely with a strong and complex intrinsic absorber. If confirmed, 4 Dra may turn out to be a key object in the study of hard X-ray emitting symbiotic stars.GALACTIC POINT SOURCES4BMUKAIKOJINULLNULLUSA5AO5THE FIRST LOOK AT THE SYMBIOTIC STAR 4 DRA ABOVE 2 KEVXISY
V2491 CYG295.767932.306867.22084844.33923679253.620655503.439016203755505.270983796340503601074400.47000074400.474400.4074400.4220210057206.557206.5158251.92PROCESSED57553.98660879635588555518.41783564823.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051213We propose to observe again one of the most luminous and intriguing classical novae of the last two years, after it has returned to quiescence. The goala are to understand how accretion is re-estabilished, investigate the claim that the white dwarf an intermediate polar (IP), estimate mass accretion are and white dwarf mass. IP are a class of X-ray sources that Suzaku is ideally suited to study, and we want to study the influence of the magnetic field on the nova evolution.GALACTIC POINT SOURCES4CORIOMARINANULLNULLUSA5AO5REVISITING AN X-RAY LUMINOUS NOVA NOVA AFTER THE ERUPTIONXISY
PSR B1259-63195.6931-63.8349304.18120501-0.990648499.869655566.836921296355569.395972222240503701090040.78000090040.790040.7090040.7220210074450.674450.6221061.81PROCESSED57600.6393755596155595.26429398153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051221We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLUSA5AO5SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011XISY
PSR B1259-63195.6913-63.8356304.18038114-0.9913128117.577355594.192766203755594.448773148240503801021478.12000021494.121478.1021494.1110110015677.415677.422111.90PROCESSED57600.79664351855597455607.12956018523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051221We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale.GALACTIC POINT SOURCES4AUCHIYAMAYASUNOBUNULLNULLUSA5AO5SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011XISY
XTE J1946+274296.420127.290663.145115651.35338176267.92555480.908680555655482.244606481540504101050731.74500050731.750731.7050731.7220210046557.146557.1115373.91PROCESSED57553.72601851855586755491.10174768523.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051231We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA5AO5-TOOCYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKUHXDY
4U 1626-67248.0734-67.4643321.7866399-13.09493758285.817255445.540925925955446.237627314840504401020033.52000020033.520057.5020045.7220210019537.219537.260179.90PROCESSED57553.30821759265582255456.23365740743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051234Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist.GALACTIC POINT SOURCES4AFINGERMARKNULLNULLUSA5AO5THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSALXISY
4U 1210-64183.3036-64.8719298.88624165-2.3008260798.495655553.159155092655555.148819444440504501079347.68000079347.679347.6079356.1220210070751.270751.2171879.90PROCESSED57554.55543981485596155595.0854745373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220512364U 1210-64 is a high mass X-ray binary with a stable 6.7 day period when the long-term (RXTE ASM) light curve is analyzed. However, we observed strong aperiodic variability in a series of pointed observations with the RXTE PCA, to the point of masking this 6.7 day period. Moreover, we have not detected a spin period, even though the accretor is most likely a neutron star. The strong variability is suggestive of accretion from a clumpy wind. We propose a 2-day Suzaku observation of this object (1) to search for unequivocal evidence for a neutron star, such as the spin period and cyclotron features; and (2) to measure the spectral shapes at different flux levels, to investigate the cause of the strong aperiodic variability.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA5AO54U 1210-64: A HIGHLY VARIABLE X-RAY BINARYXISY
4U 1728-34262.9799-33.9051354.23908298-0.18221646278.026655473.51734953755475.687696759340504801050547.210000050652.250547.2050652.2220210095360.695360.6187467.83PROCESSED57553.68844907415586755487.46626157413.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051244Fe K-alpha lines have been detected in ten NS-LMXBs. Under the commonly accepted interpretation, they can be used to set tight constrains on the accretion disk geometry. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kHz QPOs. We have recently shown that simultaneous measurements of Fe lines and kHz QPOs in a NS-LMXB appear to contradict this picture. We propose to observe 4U 1728-34 with Suzaku five times for 20 ks, simultaneously with RXTE and ATCA. This program will allow us to study and compare the dynamics of the inner edge of the disk as inferred from the Fe line and the kHz QPOs, as well as the relation of both observables with the jet radio emission.GALACTIC POINT SOURCES4ALINARESMANUELNULLNULLUSA5AO5ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES.HXDY
4U 1630-47248.5034-47.402336.903137590.24577164279.825655432.91172453755435.613425925940505101099937.310000099937.399937.3099937.3220210090451.290451.2233397.62PROCESSED57553.28496527785581555449.43695601853.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051252Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions.GALACTIC POINT SOURCES4ATOMSICKJOHNNULLNULLUSA5AO5-TOOCONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIESXISY
4U 1957+11299.842611.7251.31417386-9.3179743871.622755320.437777777855321.416805555640505701035796350003580435804035796220210030869.230869.2845800PROCESSED57551.40862268525574155375.75670138893.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051254We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind.GALACTIC POINT SOURCES4BNOWAKMICHAELNULLNULLUSA5AO54U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE?XISY
4U 1957+11299.841811.719751.31351001-9.3174505163.932555333.519027777855334.467540505702034935.33500034943.334951.3034935.3220210028262.528262.581911.80PROCESSED57551.5626504635571455347.24668981483.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051254We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind.GALACTIC POINT SOURCES4BNOWAKMICHAELNULLNULLUSA5AO54U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE?XISY
4U 1957+11299.858911.697951.30303986-9.34292333251.345955501.827546296355502.700115740740505703035349.13500035357.135349.1035357.1220210027169.727169.7753620PROCESSED57553.95206018525588155515.30150462963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22051254We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind.GALACTIC POINT SOURCES4BNOWAKMICHAELNULLNULLUSA5AO54U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE?XISY
HER X-1254.493635.271258.0664644837.48255114250.063755467.783020833355468.236296296340505801021356.72000021356.721356.7021503.4220110018932.318932.339159.90PROCESSED57553.58040509265584355477.22371527783.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052001We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?GALACTIC POINT SOURCES4BSTAUBERTR DIGERNULLNULLEUR5AO5VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1HXDN
HER X-1254.492535.270758.0656599437.48335671250.245555468.700335648255469.225891203740505802024303200002430324322.3024467.7220110022483.722483.745405.90PROCESSED57553.59174768525584855482.47269675933.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052001We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?GALACTIC POINT SOURCES4BSTAUBERTR DIGERNULLNULLEUR5AO5VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1HXDN
HER X-1254.463235.265758.0545755237.50615868268.485855461.000208333355461.449467592640505803019924200001992419924020243.8220110017507.317507.338811.90PROCESSED57553.49945601855583655470.15087962963.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052001We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?GALACTIC POINT SOURCES4BSTAUBERTR DIGERNULLNULLEUR5AO5VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1HXDN
HER X-1254.461935.265958.0546085737.50723847268.304155461.793703703755462.246747685240505804021740200002174021796021870.41101100198031980339135.90PROCESSED57553.51211805565584055474.09954861113.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052001We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity?GALACTIC POINT SOURCES4BSTAUBERTR DIGERNULLNULLEUR5AO5VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1HXDN
MU COL86.4962-32.3107237.28985275-27.1060090393.587455455.75233796355456.311354166740505901025961200002596125961025961110110021873.421873.448287.90PROCESSED57553.43810185185583655469.24523148153.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052005We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models.GALACTIC POINT SOURCES4AOSKINOVALIDIANULLNULLEUR5AO5STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKUXISY
10 LAC339.811139.061996.65409432-16.9716584281.745655344.500196759355345.069016203740506001025028.42500025028.425028.4025028.4220210021743.121743.149135.92PROCESSED57551.63932870375573155365.18243055563.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052005We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models.GALACTIC POINT SOURCES4AOSKINOVALIDIANULLNULLEUR5AO5STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKUXISY
GX 339-4255.7015-48.7852338.94105133-4.3214668883.694455603.763472222255604.234942129640506301022459.410000022459.422459.4022483.4220210019328.719328.740727.90PROCESSED57600.92446759265598355617.41206018523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052015We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4GALACTIC POINT SOURCES4ACABANACCLEMENTNULLNULLEUR5AO5-TOOPROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONSXISY
GX 339-4255.7013-48.7848338.94128957-4.3211191386.359755608.968611111155609.650196759340506302021015.72000021015.721015.7021015.7220210017595.817595.858883.90PROCESSED57600.96137731485598855621.15613425933.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052015We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4GALACTIC POINT SOURCES4ACABANACCLEMENTNULLNULLEUR5AO5-TOOPROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONSXISY
GX 339-4255.7016-48.7831338.94276391-4.3202429390.102455616.823368055655617.4487268518405063030191822000019190191980191822202100156841568454025.91PROCESSED57601.04711805565599655628.16799768523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052015We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4GALACTIC POINT SOURCES4ACABANACCLEMENTNULLNULLEUR5AO5-TOOPROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONSXISY
GX 339-4255.7013-48.7851338.94105066-4.3213014691.629655620.177870370455620.802256944540506304021799200002179921807021816.8330310018850.218850.253923.90PROCESSED57601.06240740745600955642.13103009263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052015We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4GALACTIC POINT SOURCES4ACABANACCLEMENTNULLNULLEUR5AO5-TOOPROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONSXISY
GX 339-4255.7041-48.783338.94384752-4.3214903192.895255627.546851851855628.032013888940506305016992.52000016992.520269.3020269.3220210015985.115985.141874.12PROCESSED57601.11424768525601555645.20880787043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052015We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4GALACTIC POINT SOURCES4ACABANACCLEMENTNULLNULLEUR5AO5-TOOPROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONSXISY
4U 1909+07287.70977.588341.89273161-0.82371888247.913155502.703784722255503.433773148240507301029298.22500029298.229298.2029298.2220210021391.121391.163051.90PROCESSED57553.93489583335588255515.28693287043.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22052024We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF.GALACTIC POINT SOURCES4AFUERSTFELIXNULLNULLEUR5AO5STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07XISY
SGR 0501+451675.262545.3425161.487471181.9810099982.399655459.727256944455460.989733796340507501059720.55000059808.559812.3059720.5320210052935.752935.7109065.80PROCESSED57553.49039351855528755470.14584490743.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22056002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP5AO5A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
1RXS J1708-4009257.2038-40.2142346.43162325-0.00870489267.135755466.612407407455467.773842592640507601062810.96000062818.962822.6062810.9320210059511.459511.4100323.91PROCESSED57553.56613425935528755477.27622685183.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22056002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP5AO5A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
GX 1+4263.0071-24.8161.876758654.75818757273.172755471.280127314855473.51405092594050770109967010000099670.499670099670.4320210096525.996525.9192609.10PROCESSED57553.66269675935528755487.41995370373.0.22.432Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22056002We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics".GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP5AO5A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISMHXDY
1FGL J2339.7-0531354.9077-5.546981.34836456-62.470277367.402655741.591562555743.8092361111406007010104091.4100000104091.4104091.40104099.4220210092902.292902.2191583.72PROCESSED57602.48618055565614455775.40259259263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060007We propose to observe an unidentified Fermi source (1FGL J2339.7-0531) in the first-year Fermi catalog to search for the first ``radio-quiet'' Gamma-ray emitting millisecond pulsar. The Fermi source has a candidate X-ray counterpart from Chandra data and its X-ray and Gamma-ray properties are consistent with known Gamma-ray pulsars. This system is likely in a low-mass X-ray binary system based on optical observations. Both X-ray and optical observations show clear variability. We propose to observe the Chandra source with Suzaku to search for the possible orbital period and to study its X-ray spectrum in detail. The results will provide a better insight into the high-energy emission processes in the magnetosphere of millisecond pulsars.GALACTIC POINT SOURCES4AKONGALBERTKATAOKAJUNJAP6AO6REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCEXISY
4U1812-12273.8053-12.093518.049004662.37362039267.15955838.140034722255839.916898148240600801062014.36000062014.362014.3062014.3220210053544.153544.1153509.91PROCESSED57603.32559027785622655858.31247685183.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060012Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state.GALACTIC POINT SOURCES4ASAKURAISOKINULLNULLJAP6AO6REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKUXISY
VW HYI62.2833-71.2901284.88594452-38.13999051181.981555894.100451388955895.182175925940600901070083.46000070091.470083.4070091.4220210064970.164970.193446.81PROCESSED57604.02429398155627455907.15626157413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060023SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP6AO6-TOOTOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCEXISY
VW HYI62.3036-71.2936284.88553906-38.13260514212.742755924.638379629655925.180682870440600902016159.32000016159.316159.3016159.3220210013758.713758.746851.90PROCESSED57604.26679398155631355945.91339120373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060023SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP6AO6-TOOTOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCEXISY
VW HYI62.3086-71.2914284.88209314-38.1323503276.436755986.568796296355987.250127314840600903020109.72000020109.720109.7020109.7220210020571.220571.258857.91PROCESSED57604.75909722225638556018.94178240743.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060023SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP6AO6-TOOTOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCEXISY
VW HYI62.3084-71.2978284.88912946-38.12913625338.731356049.812430555656050.166817129640600904016817.72000016825.716825.7016817.7210210013947.813947.830615.90PROCESSED57605.33128472225644956083.08570601853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060023SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate.GALACTIC POINT SOURCES4BSAITOUKEINULLNULLJAP6AO6-TOOTOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCEXISY
AQL X-1287.82710.574535.71381986-4.15705073244.526455852.154548611155853.1106254060100109494.8400009596.89494.809596.82101100353253532582587.81PROCESSED57603.46107638895624055873.12223379633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060036We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.GALACTIC POINT SOURCES4AYAMAOKAKAZUTAKANULLNULLJAP6AO6-TOOSUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASEXISY
AQL X-1287.82640.574135.71314195-4.15661165244.526855855.535798611155856.45998842594060100209940.640000100419940.6010041110110037845.137845.1798461PROCESSED57603.50739583335624155873.30255787043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060036We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.GALACTIC POINT SOURCES4AYAMAOKAKAZUTAKANULLNULLJAP6AO6-TOOSUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASEXISY
AQL X-1287.82780.571835.71173466-4.15890942243.261855858.726932870455859.578692129640601003084954000084959538.309556.6110110036476.836476.873581.92PROCESSED57603.64604166675624155874.13805555563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060036We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object.GALACTIC POINT SOURCES4AYAMAOKAKAZUTAKANULLNULLJAP6AO6-TOOSUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASEXISY
OAO1657-415255.2026-41.6667344.360190610.31327103285.901255830.398842592655832.666793981540601101084729.98000084733.784729.9084741.7220210074588.574588.5195929.72PROCESSED57603.32200231485622655858.27685185183.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060037We propose Suzaku observation of accretion-powered pulsar OAO 1657-415 to study matter accretion onto the neutron star. This object is a unique high mass X-ray binary (HMXB) that shows intermediate characteristics between wind-fed accretion pulsars and disk-fed accretion pulsars. High S/N spectra obtained by XIS, HXD-PIN/GSO with short exposure time (1 ks) allow us to investigate short-time variability of physical states of the accretion column, which is close to the neutron star surface. The proposed observation also reveals the matter distribution in the HMXB by using a 6.4-keV iron fluorescence line and hard X-rays. The data at the phase of eclipse egress provide essential information about the stellar wind and atmosphere of the companion star to constrain its stellar type in question.GALACTIC POINT SOURCES4BODAKAHIROKAZUNULLNULLJAP6AO6WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415XISY
PSR J0726-2612111.531-26.2114240.07877209-4.64696128117.998455881.569178240755882.6252546296406012010437571000004375743792043792220210039728.839728.891227.80PROCESSED57603.81726851855626455895.23880787043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060041To study the origin of magnetars, a unique opportunity is provided by detecting an excess of thermal radiation in the radio pulsars which has dipolar magnetic fields as high as magnetars. The excess is caused by field decay as seen in magnetars. A question is raised whether the rotation powered pulsars can have active magnetic flux similar to magnetars. PSR J0726-2612 is a nearby (3kpc) radio pulsar with magnetic field as high as 10^13.5 G, and therefore is an ideal target. We propose 100ksec observation of this pulsar to discover magnetar-like thermal radiation, and determine the structure of the active magnetic flux tubes by phase alignment of rotational modulation of the X-ray radiation with radio pulses.GALACTIC POINT SOURCES4CSHIBATASHINPEINULLNULLJAP6AO6CAN HIGH MAGNETIC FIELD RADIO PULSARS BE THE MAGNETAR ?XISY
CYG X-1299.591635.174571.312368223.05181611279.500155839.924502314855840.91693287044060130103702.74000038323702.7040271.8110110032962.532962.585733.91PROCESSED57603.39541666675658256212.72479166673.0.22.444Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060057We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks.GALACTIC POINT SOURCES4AYAMADASHIN'YANULLNULLJAP6AO6REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSISXISY
RXJ2056.6+4940314.192649.655989.317690972.74712249241.001155887.788680555655888.535520833340601401042373.14000042381.142373.1042373.1220210044666.544666.5645241PROCESSED57603.95033564825626455897.09947916673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060065There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources.GALACTIC POINT SOURCES4CISONAOKINULLNULLJAP6AO6SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPARTXISY
4U0114+6519.487365.3067125.698462982.5774568671.64255763.430729166755764.9453472222406017010106492.5100000106550.8106558.80106492.5220210088506.188506.1130821.91PROCESSED57602.65184027785615255785.04439814823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060071We propose to observe an X-ray pulsar, 4U 0114+65 for 100 ks. This object is known to be a neutron star binary with an orbital period of 12 days and a long pulse priod of 10 ks. Our goals are to obtain time-averaged spectra of the XIS and HXD, and to quantify spectral changes between flare and quiescense phases, and to search for a cyclotron absorption line around ~ 60 keV. We also study pulse-phase resolved spectra. With these pieces of information, we aim at clarifying whether this source is a magnetar descendent or a neutron star with ordinary magnetic fields.GALACTIC POINT SOURCES4ASASANOMAKOTONULLNULLJAP6AO6SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIESXISY
1RXSJ175911.0-344921269.7922-34.8194356.38251758-5.4610223872.120555993.902951388955994.91265046340601901040181.34000040181.340181.3040181.32202100347513475187233.91PROCESSED57604.83585648155638556016.66807870373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060085We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates.GALACTIC POINT SOURCES4CMORIHIDEYUKINULLNULLJAP6AO6SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
24M2791334.957763.2629106.818770195.23758822230.000855947.370451388955948.092638888940602301034601.73000034617.734601.7034609.7220210035059.535059.562391.90PROCESSED57604.50878472225634055973.11028935183.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060087We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object.GALACTIC POINT SOURCES4COHNOMASANORINULLNULLJAP6AO6SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCESXISY
1FGL J1715.2-3319258.713-33.4282352.626846013.0177452599.073756002.562916666756003.375081018540602401032165300003216532165032165220210027984.827984.8701660PROCESSED57604.92960648155638656019.25164351853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060087We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object.GALACTIC POINT SOURCES4COHNOMASANORINULLNULLJAP6AO6SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCESXISY
AXP 4U 0142+61426.568261.7591129.37061357-0.4252315840.38455811.655231481555812.573113425940603101038649.76000038649.738649.7038682.5220210042196.442196.4792920PROCESSED57603.12201388895621855851.44068287043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060092We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI.GALACTIC POINT SOURCES4ANAKAGAWAYUJINNULLNULLJAP6AO6-TOOA SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONSXISY
RS OPH267.5535-6.695119.8101108210.3796703294.907255987.260879629655988.855406033010693861000006938669386069386220210060089.960089.9137719.80PROCESSED57604.83008101855637556008.3242245373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060096We propose a 100 ks observation of a recurrent novae remnant RS Ophiuchi. Using Suzaku's wide-energy coverage and excellent spectral performance, we aim to diagnose plasma and to discover non-thermal emission at a recurrent novae remnant.GALACTIC POINT SOURCES4CTAKEIDAINULLNULLJAP6AO6OBSERVATION OF A RECURRENT NOVA REMNANT RS OPHIUCHIXISY
1RXSJ013106.4+61203522.761961.3591127.66105316-1.1484194576.812955765.703217592655766.018206018540603401013296.32000013296.313296.3013296.3110110015882.915882.927199.90PROCESSED57602.64248842595637455784.98864583333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060097We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.GALACTIC POINT SOURCES4BTAKAHASHIHIROMITSUNULLNULLJAP6AO6SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATESXISY
1RXSJ013106.4+61203522.803261.3371127.68400105-1.16712133215.002555993.566493055655993.88983796340603402012173.7800012173.712173.7012173.72202100178971789727921.90PROCESSED57604.80115740745637456008.11917824073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060097We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.GALACTIC POINT SOURCES4BTAKAHASHIHIROMITSUNULLNULLJAP6AO6SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATESXISY
1RXSJ194246.3+103339295.697610.539948.24168916-6.37340779280.000255848.143356481555848.63562540603501020488.92000020488.920488.9020488.932021001714217142425080PROCESSED57603.41895833335624055873.00048611113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060097We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.GALACTIC POINT SOURCES4BTAKAHASHIHIROMITSUNULLNULLJAP6AO6SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATESXISY
1RXSJ135341.1-664002208.4233-66.67309.05087215-4.54070575288.531455774.159305555655774.693923611140603601023267.92000023275.923267.9023275.9110110022424.122424.146183.90PROCESSED57602.71241898155616655802.46284722223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22060097We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray.GALACTIC POINT SOURCES4BTAKAHASHIHIROMITSUNULLNULLJAP6AO6SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATESXISY
HD162020267.6611-40.3282350.73095661-6.73195128265.86755808.091956018555808.407870370440603701015922.91500015922.915922.9015922.9110110015940.615940.627287.92PROCESSED57603.05709490745623255865.11599537043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
HD162020267.6612-40.3294350.72995016-6.73261971268.334355816.413229166755816.72796296340603702015036.21500015044.215044.2015036.2220210015582.915582.927183.90PROCESSED57603.11943287045621855851.43944444443.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
HD162020267.6618-40.3275350.73183598-6.73206134259.998755824.649895833355825.163240740740603703016230150001623816238016230220210013378.413378.444345.91PROCESSED57603.19880787045621855851.44748842593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
HD162020267.6661-40.3245350.73610578-6.73339029259.998655833.025520833355833.427951388940603704016729.71500016737.716737.7016729.7110110015728.615728.634749.90PROCESSED57603.27283564825622555858.13974537043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
HD162020267.6578-40.3138350.74222411-6.72254511106.35256005.853506944456006.062615740740603801010428.61000010437.310437.3010428.611011007673767318055.90PROCESSED57604.96101851855643556068.6254745373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
HD162020267.6599-40.3316350.72753331-6.73286722269.501855820.467245370455820.6918634259406038020889610000889688960889611011007851.97851.919399.90PROCESSED57603.16768518525621855851.44440972223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
HD162020267.6631-40.3218350.73730077-6.73005667259.998755829.42421296355829.65438657414060380301148110000114811148101148111011008540.28540.219879.90PROCESSED57603.24076388895622555858.07901620373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061202Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction.GALACTIC POINT SOURCES4APILLITTERIIGNAZIONULLNULLUSA6AO6STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS.XISY
ETA CARINAE161.2639-59.6881287.59810122-0.63296206310.012255766.032939814855766.928622685240603901042030.25000042030.242030.2042030.2110110049093.749093.777383.90PROCESSED57602.66254629635616355785.02817129633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061205Eta Car is the nearest highly unstable extremely massive star and a key object for understanding how mass and angular momentum change as an extremely massive star heads towards hypernova. Periodic minima in X-rays and other wavebands show it as an extremely eccentric binary with a massive companion. A surprising change in the X-ray emission during the January 2009 X-ray minimum probably indicates a large-scale variation in the LBV primary's mass loss rate. We propose a Suzaku observation in AO6 to monitor the change of the absorption column in the line of sight and the non-thermal emission above 10 keV. The observation will help to study geometry of the binary orbit of Eta Car and the mechanism of the non-thermal emission.GALACTIC POINT SOURCES4BHAMAGUCHIKENJINULLNULLUSA6AO6MONITORING DYNAMICAL MASS LOSS FROM ETA CAR WITH SUZAKU: APASTRONXISY
GAMMA CASSIOPEIAE14.159860.7356123.56796459-2.1297251172.508455755.003888888955756.33358796340604001055394500005539455394055394220210056216.456216.4114877.80PROCESSED57602.60197916675618355816.66552083333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061207We propose a 50 ks Suzaku observation to obtain for the first time the hard X-ray spectrum of the classical Be star Gamma Cas. This star is a prototype of the "Gamma Cas stars" class, whose nature is not yet understood. Earlier XMM-Newton and Swift BAT observations gave a hint of the presence of the hard X-ray emission above 10 keV. The broadband Suzaku spectrum will allow to establish its X-ray emission mechanism - non-thermal emission or reflection of thermal emission from a neutral surface. On this basis, we will be able to discriminate the mechanisms between the magnetic disk dynamo and the accretion on a compact star. These new data will be pivotal in solving the enigma of Gamma Cas and revealing the true nature of this astrophysically important object.GALACTIC POINT SOURCES4CHAMAGUCHIKENJINULLNULLUSA6AO6SUZAKU'S HARD LOOK AT GAMMA CASSIOPEIAEXISY
4 DRA187.565569.216125.7255184547.79722512145.531855874.170729166755875.061932870440604101042258400004225842258042258220210039792.539792.5769982PROCESSED57603.72105324075626055890.69614583333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V220612124 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA6AO6A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTIONXISY
V1082 SGR286.8363-20.772115.88147607-12.6753541281.381856009.184814814856010.445937540604201039460.54000039460.539460.5039460.5220210036017.136017.11089242PROCESSED57605.00885416675639956023.15642361113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061217V1082 Sgr is a BAT-detected cataclysmic variable with a 20 hr orbital period that exhibits high and low states. The high X-ray luminosity and the presence of the HeII 4686 lines in its optical spectrum have led to the suggestion that this is an intermediate polar (IP). We propose an exploratory 40 ks Suzaku observation with the aim of establishing if it is indeed an IP. If it is, then this system may provide a unique opportunity to study an IP in a low state, which has not been possible with other IPs.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA6AO6AN UNUSUAL BAT-DETECTED CATACLYSMIC VARIABLE, V1082 SGRXISY
4U 1954+31298.933432.080368.380771311.91321277261.256255857.337326388955858.720300925940604601060216600006022460232060216320210057900.857900.8119467.90PROCESSED57603.61599537045624155874.10693287043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061226We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios.GALACTIC POINT SOURCES4BENOTOTERUAKINULLNULLUSA6AO6THE SLOWEST ROTATING PULSAR 4U 1954+31XISY
4U 0115+6319.620963.7559125.916700351.0409995484.716755747.002743055655748.052997685240604801024279500002428024279024283.9220210045127.245127.290727.91PROCESSED57602.52011574075616355778.42986111113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061234We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA6AO6-TOOCYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELDXISY
4U 0115+6319.613963.7554125.913673851.0401780682.123555750.05358796355751.021076388940604901042274.84500042274.842354.8042354.8220210042143.242143.283577.91PROCESSED57602.55776620375616355778.43112268523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061234We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA6AO6-TOOCYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELDXISY
GX 304-1195.3153-61.5986304.100019531.25086712115.933855957.43703703755959.166944444440606001016524.36500016691.216524.3016691.2220210058712.458712.4149432.13PROCESSED57604.55231481485639956033.26950231483.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061235We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma.GALACTIC POINT SOURCES4APOTTSCHMIDTKATJANULLNULLUSA6AO6-TOOCYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINESXISY
SGR 1806-20272.1607-20.400810.00344249-0.2343365789.033456010.44983796356012.531481481540606901070596.47000070596.470596.4070596.4220210063957.163957.1179827.92PROCESSED57605.05004629635639956023.23873842593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22061301Recent Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic ages. The hard X-rays of magnetars become weaker but harder for older objects. In order to accomplish this picture, we have to verify that this correlation is rather free from selection effects, and holds even when the sources vary on long time scales. Here we propose a 70 ks observation of SGR 1806-20. If we detect the hard X-rays from this source at a rather intensity, the above correlation will be much reinforced.GALACTIC POINT SOURCES4CENOTOTERUAKINULLNULLUSA6AO6VARIABILITY OF HARD X-RAYS FROM MAGNETARSXISY
GX 17+2274.0108-14.048216.424013511.2676957264.771555853.11609953755855.52870370374060700106506.91000006757.26506.906757.2320210087359.987359.9208429.73PROCESSED57603.52700231485624155873.29444444453.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22062003The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique.GALACTIC POINT SOURCES4ACACKETTEDWARDNULLNULLEUR6AO6EXPLORING THE IRON LINE - KHZ QPO CONNECTIONXISY
4U 1543-624236.9719-62.5774321.74901084-6.34183385299.193955826.405682870455827.621759259340607201049185.15000049193.149185.1049201.1220210045309.445309.4105059.91PROCESSED57603.25646990745622255851.45561342593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22062010We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results.GALACTIC POINT SOURCES4AMADEJOLIWIANULLNULLEUR6AO6INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624XISY
AX J1818.8-1559274.7184-16.000215.02984997-0.2600064265.851755849.553888888955852.147453703740607401095191.210000099385.999385.9095191.2220210083874.683874.6224069.91PROCESSED57603.49003472225624155873.9935995373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22062016The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidatesGALACTIC POINT SOURCES4BMEREGHETTISANDRONULLNULLEUR6AO6A NEW GALACTIC MAGNETAR CANDIDATEXISY
4U 1705-44257.2257-44.096343.32512852-2.33758895104.995556013.532048611156016.4231134259406076010100811.2100000100811.2100819.20100820.9220210090075.990075.9249767.72PROCESSED57605.10224537045639356027.20136574073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22062019We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system.GALACTIC POINT SOURCES4ADI SALVOTIZIANANULLNULLEUR6AO6-TOOSUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATEXISY
IGRJ16479-4514252.0242-45.1934340.16807688-0.1166845991.531755980.943819444455983.5363541667406078010149778.5150000149786.5149778.50149786.52202100154729.5154729.5223981.90PROCESSED57604.80638888895642956062.27884259263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22068014We propose a 100 ks observation of the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period, the eclipsing IGRJ16479-4514 (3.3 d), with the main aim of probing its X-ray properties along one entire orbital phase with unprecedented sensitivity. The requested net exposure time indeed translates into an observation almost continuously spanning the whole binary system orbit, allowing for the first time an orbital phase resolved investigation of the X-ray emission properties, which will allow us to study the structure of the supergiant companion (its density and ionization state) and to cast light on the outburst mechanism at work in this new class of transients.GALACTIC POINT SOURCES4ASIDOLILARABODAGHEEARASHEUS6AO6UNVEILING THE MYSTERY OF THE SUPERGIANT FAST X-RAY TRANSIENT WITH THE SHORTEST ORBITAL PERIODXISY
H1743-322266.5676-32.2352357.25483145-1.83570092273.687756204.782280092656205.607824074140700501020811400002081120811020811220210042433.742433.771321.90PROCESSED57607.29603009265659556226.55962962963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070002Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP7AO7-TOOMULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
H1743-322266.5662-32.2338357.25541352-1.83396197273.688156210.646226851856211.586273148240700502021192.24000021192.221192.2021192.23202100415174151781215.92PROCESSED57607.74473379635659556226.58822916673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070002Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP7AO7-TOOMULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
H1743-322266.5672-32.235357.25482673-1.83530791277.971356212.404988425956213.3744560185407005030213614000021370.621372.202136133031004061540615837361PROCESSED57607.73854166675659856232.4732754633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070002Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP7AO7-TOOMULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
HEN 3-461159.7779-51.4088282.902695166.2428626116.171556278.133634259356278.90640046340700701045734.84000045734.845734.8045734.8220210046677.446677.466761.90PROCESSED57608.30719907415601856303.55059027783.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070021Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects.GALACTIC POINT SOURCES4CEZEROMANUSNULLNULLJAP7AO7SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARSXISY
MRK 520330.176810.54569.38972894-34.038497250.500256258.818645833356260.657141203740701401079779.58000079779.579787.5079795.522021007764177641158825.81PROCESSED57608.15232638895664456275.72555555563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070028Compton-thick AGNs contribute to the hard X-ray background and are key objects for investigating the cosmological evolution of AGNs. But heavy obscuration under 10 keV, and source misidentification mean that very few sources have been studied in detail. We have developed new infrared and hard X-ray diagnostics of AGN identification, based on which we select one candidate, Mrk 520, which must be very highly obscured and likely Compton-thick. With Suzaku, we will characterize all emission components, not only thermal and scattering components under 10 keV, but also the heavily obscured continuum over 10 keV, and reflection components.GALACTIC POINT SOURCES4CMATSUTAKEIKONULLNULLJAP7AO7MRK 520 : A NEW COMPTON-THICK AGN?XISY
CYG X-1299.587535.203171.335065793.0695777688.780256390.095347222256391.95855324074070150104149.98500085034149.9066475.1210110071712.871712.8160965.83PROCESSED57611.20468755680856402.13910879633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070030We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes.GALACTIC POINT SOURCES4AYAMADASHINYANULLNULLJAP7AO7INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1XISY
CYG X-1299.578735.202471.33071593.075350859.569156419.092557870456419.60716435184070150201512.4200003244.21512.4021480220110020925.820925.8444580PROCESSED57611.26253472225680856442.97155092593.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070030We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes.GALACTIC POINT SOURCES4AYAMADASHINYANULLNULLJAP7AO7INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1XISY
Z CAM126.373.123141.3686197332.6242474591.204356239.036898148256239.780034722240701601035852350003585235852035852220210033896.833896.864193.91PROCESSED57607.97973379635663156264.6023495373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070038Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases.GALACTIC POINT SOURCES4CSAITOUKEINULLNULLJAP7AO7COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCEXISY
AX J1622.1-5005245.5334-50.0932333.60606211-0.20489946274.381256160.996840277856161.939814814840701801039126.34000040536.640536.6039126.32202100374763747681461.90PROCESSED57606.93178240745666756300.56377314823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070043Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP7AO7ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?XISY
AX J1846.8-0240281.7182-2.661330.04319345-0.1985098989.405756018.012511574156019.114699074140701901037620.94000037620.941612.7039220.72202100372503725095219.90PROCESSED57605.07569444455640056033.23230324073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070043Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP7AO7ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?XISY
AX J1620.7-4942245.1985-49.7112333.723069760.21790295274.600456158.520902777856159.524571759340702001042206.24000044271.344274.4042206.2320310044805.244805.286711.90PROCESSED57606.898755658256212.77899305563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070043Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP7AO7ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?XISY
AX J1445.7-5931221.4519-59.5275316.977804190.18867801281.52656143.282951388956144.291886574140702101040052.54000041068.241060.2040052.5210210036808.936808.987157.91PROCESSED57606.74597222225653356167.21163194443.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070043Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution.GALACTIC POINT SOURCES4AMAKISHIMAKAZUONULLNULLJAP7AO7ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS?XISY
1RXSJ170047.8-314442255.196-31.7452352.212293566.4002075790.794456341.493206018556341.75012731484070270108926.2120008926.28926.208926.2220210082328232221860PROCESSED57610.62258101855671856352.49864583333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070052We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4CMORIHIDEYUKINULLNULLJAP7AO7SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ173905.2-392615264.7748-39.4365350.35081336-4.37467046271.200656188.823738425956189.344699074140702901022063.81500022071.822063.8022071.8110110018251.518251.544999.90PROCESSED57607.08918981485658456218.49942129633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070052We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4CMORIHIDEYUKINULLNULLJAP7AO7SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
U GEM IN QUIECSECNCE118.77721.9977199.2288200223.39765052280.87956041.563692129656044.5765856482407034010119113.6120000119113.6119113.60119113.63202100102835.4102835.42603061PROCESSED57605.34960648155643456068.62283564823.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070065It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission.GALACTIC POINT SOURCES4BHAYASHITAKAYUKINULLNULLJAP7AO7-TOOOBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURSTXISY
U GEM IN OUTBURST118.773221.9928199.2324125923.39259554281.11756029.410532407456030.75016203740703501050254.75000050254.750254.7050254.7220210047296.747296.7115707.91PROCESSED57605.20021990745641556044.38877314823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070065It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission.GALACTIC POINT SOURCES4BHAYASHITAKAYUKINULLNULLJAP7AO7-TOOOBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURSTXISY
IGR J17091-3624257.2866-36.4073349.527010922.20940495283.891556202.863668981556203.720266203740703701042075.912000042075.942083.7042079.73303100403924039274007.90PROCESSED57607.26600694445672856226.67013888893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070097We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate.GALACTIC POINT SOURCES4BYAMAOKAKAZUTAKANULLNULLJAP7AO7SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624XISY
IGR J17091-3624257.2807-36.4071349.524342082.2133388590.724556342.706516203756344.885682870440703702081946.78000081946.781946.7081946.7220210072871728711882601PROCESSED57610.69442129635672856363.61469907413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070097We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate.GALACTIC POINT SOURCES4BYAMAOKAKAZUTAKANULLNULLJAP7AO7SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624XISY
II PEG358.774428.6284108.23861581-32.63076231231.141156301.187731481556303.648796296340703801017017.6100000111506.5111514.5017017.63303100107905.8107905.8212619.82PROCESSED57608.50743055565672456363.6020370373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070102We propose a Suzaku observation of the powerful flare star II Peg with the high sensitivity of HXD. MAXI/GSC results from 2009 to 2011 show that this source exhibits the highest flaring activity with the largest luminosities and the largest fluxes. Then detection of the non-thermal emission is the most expected from this source at the on-set of a flare. We are to observe this target simultaneously with radio, infrared, optical, and X-ray bands for the first time. Our goal is (1) to detect impulsive non-thermal emission at the powerful II Peg flare (2) to obtain wide-band SED variability from radio to hard X-ray band, and (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band.GALACTIC POINT SOURCES4CTSUBOIYOHKONULLNULLJAP7AO7NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEGXISY
EUVE J1439 +75.0219.945975.0823114.1124905940.13551871340.489756067.288472222256067.859942129640703901029961.34000029969.329969.3029961.3110110032393.232393.249343.90PROCESSED57605.47575231485644256076.0289120373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070112The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects.GALACTIC POINT SOURCES4BHARAYAMAATSUSHINULLNULLJAP7AO7SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFSXISY
PG 1658 +440254.934844.009469.1116717138.06633743330.999856115.674097222256116.830104166740704001051032.95000051032.951032.9051032.9110110046674.646674.699871.81PROCESSED57606.58972222225650856142.14473379633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22070112The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects.GALACTIC POINT SOURCES4BHARAYAMAATSUSHINULLNULLJAP7AO7SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFSXISY
WR140305.137443.847580.932937924.16074264212.527256283.352835648256284.208530092640704101054780.25000054796.254780.2054804.2320310052381.152381.1739200PROCESSED57608.33969907415671056344.69616898153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071203In the campaign observations of the prototypical colliding wind binary system WR 140 at its last periastron passage in 2009, Suzaku discovered an extremely hard and variable X-ray component. The current best explanation of its origin is inverse-Compton cooling of particles accelerated in the wind-wind collision shock, and if so this would be the first detection of non-thermal X-ray emission from any Wolf-Rayet system. However, other mechanisms cannot be excluded because the observed intensity was stronger than expected from the observed radio luminosity. We propose to re-observe WR 140 near apastron in 2012 with Suzaku to identify the emission mechanism which produces the hard component.GALACTIC POINT SOURCES4CHAMAGUCHIKENJINULLNULLUSA7AO7MEASURING EXTREMELY HARD X-RAY EMISSION FROM WR140 AT APASTRONXISY
HEN 3-1591271.8863-25.89815.07192211-2.68044312269.642156203.724953703756204.779398148240704201051387.65000051387.751387.6051403.6430310052368.152368.191095.91PROCESSED57607.28998842595659256226.55456018523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071211The number of symbiotic stars known to be medium energy (2-10 keV) X-ray emitters has increased markedly in the last several years. These are white dwarfs accreting from a giant mass donor, unlike the less common class of symbiotic X-ray binaries in which the accretor is a neutron star. The X-ray spectra of the white dwarf symbiotics can be used to constrain the white dwarf mass and accretion rate. Here we focus on one object, Hen 3-1591, which belongs to a rare subclass of d'-type yellow symbiotic, commonly thought to harbor a young white dwarf. Hen 3-1591 is the first of this subclass to show medium energy X-ray emission, and hence we propose a moderately deep Suzaku observation to characterize its white dwarf and the circum-binary environment.GALACTIC POINT SOURCES4BMUKAIKOJINULLNULLUSA7AO7THE X-RAY EMISSION OF THE YELLOW SYMBIOTIC STAR, HEN 3-1591XISY
CH UMA151.745767.5324142.9125656242.65793237289.997956048.500949074156049.481504629640704301045204.54000045204.545204.5045204.5220210043375.143375.184698.10PROCESSED57605.32496527785643556068.62461805563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071212The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates?GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLUSA7AO7DWARF NOVAE WITH EXTREME WHITE DWARF MASSESXISY
EK TRA228.5098-65.0893317.22984637-6.25468419278.600256149.738715277856150.847361111140704401077834.47000077850.477834.4077850.4220210069897.369897.395777.92PROCESSED57606.84949074075654056170.03605324073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071212The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates?GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLUSA7AO7DWARF NOVAE WITH EXTREME WHITE DWARF MASSESXISY
BF ERI69.8754-4.5962201.0367912-31.29845078262.013356350.919062556351.625300925940704501032817.73000032817.732817.7032817.8330310032016.132016.161009.91PROCESSED57610.69300925935673856372.51387731483.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071212The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates?GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA7AO7DWARF NOVAE WITH EXTREME WHITE DWARF MASSESXISY
BV CEN202.8234-54.9803308.679031837.44609562120.716756329.024687556329.485601851840704701033380300003338833388033380110110030869.230869.239815.90PROCESSED57610.52622685185671556349.48469907413.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071212The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates?GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA7AO7DWARF NOVAE WITH EXTREME WHITE DWARF MASSESXISY
T PYXIDIS136.1704-32.3688257.197273029.71237496121.994356266.27266203756268.8695486111407048010866761000008667686676086676220210073611.873611.8224357.94PROCESSED57608.2495254635666056291.82307870373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071213We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins.GALACTIC POINT SOURCES4CTAKEIDAINULLNULLUSA7AO7COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTSXISY
HERCULES X-1254.460535.328858.1326418637.51848299268.799956189.353831018556190.030023148240705101025535.62000025543.625549.4025535.6220210025087.925087.958421.90PROCESSED57607.10170138895659056218.52284722223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071224This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star.GALACTIC POINT SOURCES4BGREFENSTETTEBRIANNULLNULLUSA7AO7STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITYXISY
HERCULES X-1254.460535.328858.1326418637.51848299268.399956192.181134259356192.78141203740705102022609.42000022609.422609.4022609.4320210020178.720178.7518361PROCESSED57607.165659056218.57269675933.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071224This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star.GALACTIC POINT SOURCES4BGREFENSTETTEBRIANNULLNULLUSA7AO7STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITYXISY
HERCULES X-1254.461235.32958.1330062637.51795138268.199856194.431770833356195.064108796340705103023589.42000023593.123593.1023589.4220210023476.923476.9546340PROCESSED57607.19456018525668956323.51487268523.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071224This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star.GALACTIC POINT SOURCES4BGREFENSTETTEBRIANNULLNULLUSA7AO7STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITYXISY
4U1538-522235.6015-52.3857327.421889542.16239803275.297256149.003113425956149.734953703740706801045955.44000045955.445955.4045955.422021004005040050632120PROCESSED57606.82694444445664056272.6889004633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071233Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit.GALACTIC POINT SOURCES4AROTHSCHILDRICHARDNULLNULLUSA7AO7THE FIRST SUZAKU OBSERVATION OF 4U1538-522XISY
1FGL J1018.6-5856154.7397-58.9449284.35462729-1.68677577302.897456098.929861111156100.461238425940706901072841.27000072841.272841.2072841.2220210057677.357677.31322500PROCESSED57605.77910879635647956113.2589004633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071234We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation.GALACTIC POINT SOURCES4BTANAKATAKAAKINULLNULLUSA7AO7SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856XISY
1FGL J1018.6-5856154.7377-58.9433284.35288518-1.68600623306.34256102.988240740756103.369687540707001017447.32000017464.517463.3017447.3220210014447.414447.432949.92PROCESSED57606.48347222225648056114.17193287043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071234We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation.GALACTIC POINT SOURCES4BTANAKATAKAAKINULLNULLUSA7AO7SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856XISY
1FGL J1018.6-5856154.7369-58.9465284.35429996-1.68890631297.836756093.024687556093.534803240740707101020820.32000020820.320820.3020820.32202100168131681344063.90PROCESSED57605.67792824075654256176.2370254633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071234We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation.GALACTIC POINT SOURCES4BTANAKATAKAAKINULLNULLUSA7AO7SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856XISY
CYGNUS X-1299.596935.189171.327107593.05572664254.870156231.341678240756232.109212963407072010372.6300001939.41990.80372.6110110030085.730085.766305.90PROCESSED57607.94274305565661156245.51074074073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22071241We propose for a single 30 ks observation of the accreting black hole Cygnus X-1. NuSTAR is an upcoming (to be launched in Spring 2012) hard X-ray (5-80 keV) mission that will plan its schedule to obtain simultaneous coverage of Cyg X-1 with Suzaku. The observations will be used for both science and cross-calibration. The combination of Suzaku and NuSTAR will provide the best measurement of the reflection component, including a relativistically broadened iron line and a hard X-ray excess, and the information will be used to test emission models and constrain the Cyg X-1 accretion geometry. The XIS capabilities to measure the iron line are essential for the science, and the HXD coverage is essential for the cross-calibration.GALACTIC POINT SOURCES4ATOMSICKJOHNNULLNULLUSA7AO7CYGNUS X-1 WITH SUZAKU AND NUSTARXISY
LMC X-384.7483-64.0713273.56080053-32.07680965285.800856379.676944444556382.47936342594070860101018091000001018171018250101809220210092724.692724.6242101.91PROCESSED57611.01695601855675756391.80675925933.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072002We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state.GALACTIC POINT SOURCES4AKOLEHMAINENMARINULLNULLEUR7AO7-TOOA TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES?XISY
4U 0352+3058.842731.0494163.07655547-17.1355363377.700256166.36015046356170.0980208333407088010153489.3150000153489.3153489.30153489.32202100140991.9140991.9322923.63PROCESSED57607.06372685185658256212.76097222223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072011After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys.GALACTIC POINT SOURCES4BDOROSHENKOVICTORNULLNULLEUR7AO7CRACKING THE X PERXISY
EXO 2030+375308.046237.655577.15821576-1.2199782258.311356070.842071759356072.78984953740708901077945.17500077953.177956.9077945.121021007251572515168255.80PROCESSED57605.54253472225644956083.20888888893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072013We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties.GALACTIC POINT SOURCES4AFERRIGNOCARLONULLNULLEUR7AO7UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375XISY
J1620-4927245.1748-49.4572333.891096560.40900491274.300256157.802951388956158.520335648240709101029260.12500029260.129284.1029260.1110110029840.229840.261967.90PROCESSED57606.87168981485659256226.60981481483.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072019The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.GALACTIC POINT SOURCES4AMARELLIMARTINONULLNULLEUR7AO7SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARSXISY
J1803-2149270.7914-21.81848.142419870.18738401269.700556191.337164351856192.173067129640709201031998.62500032021.832014.6031998.6220210028881.228881.272217.91PROCESSED57607.12767361115658456218.55342592593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072019The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.GALACTIC POINT SOURCES4AMARELLIMARTINONULLNULLEUR7AO7SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARSXISY
J1746-3239266.7261-32.6662356.95543166-2.1735171272.015356365.646967592656366.402245370440709301027346.92500027346.927346.9027346.92202100270052700565251.92PROCESSED57610.82160879635674556379.5307754633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072019The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.GALACTIC POINT SOURCES4AMARELLIMARTINONULLNULLEUR7AO7SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARSXISY
J1522-5734230.5286-57.5816322.05619938-0.4156844274.497156154.648634259356155.007835648240709401030029.52500030045.530029.5030045.5110110023686.223686.231023.90PROCESSED57606.85381944445663856272.66472222223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22072019The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances.GALACTIC POINT SOURCES4AMARELLIMARTINONULLNULLEUR7AO7SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARSXISY
1FGL J1018.6-5856154.7461-58.9386284.35392298-1.67969789308.62256105.712418981556106.652361111140709601060432.46000060432.460432.4060432.4220210053597.853597.881205.91PROCESSED57606.51247685185648456118.04965277783.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22073113Recently, a modulated signal has been detected with the Fermi from the source 1FGL J1018.6-5856. The presence of a O-type star in this source, and the variable character of the signal suggested that the source is a new gamma-ray binary system. Since it is expected that X-rays in these sources has the synchrotron origin, detailed X-ray observations are very important for understanding of the processes occurring in the system. However, sensitive observations of source in the X-ray energy bands are still missing. Therefore, we propose to observe the source with Suzaku. Since a long observational campaign is planned for 2012 by the HESS collaboration, the obtained X-ray, together with TeV, data will allow a proper modeling of the physical processes behind the non-thermal emission in system.GALACTIC POINT SOURCES4BODAKAHIROKAZUTANAKATAKAAKIJUS7AO7X-RAY OBSERVATION OF GAMMA-RAY BINARY 1FGL J1018.6-5856XISY
V4641 SGR274.8371-25.40526.77442002-4.7857171484.000456741.973715277856744.895972222240800201049223.710000049223.749270.6049224.2330310089743.989743.9252455.61PROCESSED57614.16322916675719056821.86855324073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080009We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics: 1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, MAXI/GSC, Swift/XRT and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planned simultaneously with Swift, many radio and optical/NIR observatories.GALACTIC POINT SOURCES4AYAMAOKAKAZUTAKANULLNULLJAP8AO8-TOOTHE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGRXISY
CRAB PULSAR83.630222.0185184.55261516-5.7844761387.462856551.70359953756552.187650463408008010248.320000248.3248.30248.32202100163121631241817.91PROCESSED57612.63494212965695656588.6035995373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080026We hereby submit a proposal for Suzaku/HXD observations of the Crab pulsar' hard X-ray pulses, which will be coordinated with simultaneous detection of giant radio pulses at ground radio telescopes. With these observations, we will get a statistically significant confirmation (or denial) of the existence of correlation between X-ray intensity and giant radio pulses, which has been found, with a marginal significance, during our trial observations of the Crab pulsar in which we utilized the calibration data of the HXD. If this correlation is confirmed, a new insight into the physics of pulsars' magnetospheres can be obtained.GALACTIC POINT SOURCES4CTERASAWATOSHIONULLNULLJAP8AO8CORRELATION STUDY OF X-RAY PULSES AND GIANT RADIO PULSES FROM CRAB PULSAR WITH SUZAKU/HXDXISY
4U 0614+09194.27889.1363200.87717258-3.3652294489.799556579.422731481556580.831435185240800901033687600003368734647.4034936.6340410057701.657701.6121663.90PROCESSED57612.97153935185714456601.61447916673.0.22.444Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080028We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB.GALACTIC POINT SOURCES4BSUGITASATOSHINULLNULLJAP8AO8THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATEXISY
4U 0614+09194.28269.1348200.88027144-3.36263018270.722756737.098229166756738.458425925940800902015668.96000015831.415668.9015820.5430310060557.460557.4117501.82PROCESSED57614.07871527785714456778.68096064823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080028We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB.GALACTIC POINT SOURCES4BSUGITASATOSHINULLNULLJAP8AO8THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATEXISY
4U 0142+6126.583861.7628129.37704782-0.420057282.99756504.420590277856506.6252430556408011010101167.8100000101167.8101182.80101182.82202100102473.9102473.9190463.71PROCESSED57612.15586805565695356587.50596064823.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080035A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61.GALACTIC POINT SOURCES4AENOTOTERUAKINULLNULLJAP8AO8TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSIONXISY
SGR 0501+451675.277445.2864161.538212281.9548303687.705456535.976157407456536.875266203740801301036124.44000036124.441261.1041245.2220110035717.735717.777671.91PROCESSED57612.4593755697456608.65863425933.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080040Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.GALACTIC POINT SOURCES4BENOTOTERUAKINULLNULLJAP8AO8ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACYXISY
SGR 1806-20272.1614-20.40729.99816367-0.2380141988.252157120.824259259357122.740532407440801401070819.57000070819.574773.9074816.922030000000PROCESSED57618.00341435185750357135.38283564823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080040Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.GALACTIC POINT SOURCES4BENOTOTERUAKINULLNULLJAP8AO8ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACYXISY
SWIFT J1834.9-0846278.7285-8.772423.24882887-0.35409613264.998656582.304131944456583.333530092640801501035931.74000038111.738111.7035931.7220310031926.431926.488931.91PROCESSED57613.01487268525696756601.63099537043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080040Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources.GALACTIC POINT SOURCES4BENOTOTERUAKINULLNULLJAP8AO8ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACYXISY
SAGITTARIUS A*266.4197-29.0062359.94692786-0.04746309282.004356539.531041666756540.00016203740801701019457.92000019478.919457.9019470.9220210020642.320642.340521.90PROCESSED57612.48549768525697456608.64939814823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4166-29.0014359.94961276-0.04264831285.005856547.259733796356547.6558101852408017020192762000019282.319290.1019276330310021083.421083.4342180PROCESSED57612.60337962965695656588.74621527783.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4172-29.0091359.94331347-0.04710749285.001556554.856608796356555.443993055640801703020261.3200002026820261.30202682202100205492054950741.91PROCESSED57612.65582175935695656588.69289351853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4179-29.0156359.938084-0.05101613284.996756561.900810185256562.482858796340801704018328.52000018342.218328.5018342.2320310018951.918951.9502820PROCESSED57612.72445601855695656588.49722222223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4147-29.0052359.94550345-0.04320951106.999556723.056527777856723.548738425940801705021994.92000021994.922002.9022014.41101100158621586242519.91PROCESSED57613.97068287045710056734.64443287043.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4146-29.0065359.94434823-0.0438121107.000156728.647453703756729.114756944540801706021138.72000021142.721138.7021159.5220310020484.420484.4403680PROCESSED57614.00782407415711356747.65409722223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.415-29.0052359.94564014-0.04343346106.999856738.472418981556738.989768518540801707021588.72000021618.521588.7021644.222021001927419274446940PROCESSED57614.08336805565712056750.82122685183.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.415-29.006359.94495727-0.04385023107.000456744.900752314856745.623854166740801708020481.82000020491.720503.6020481.8330310019749.819749.862471.91PROCESSED57614.13848379635712156756.76351851853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4154-29.0072359.94411521-0.04477398105.69956752.45140046356752.984861111140801709022166.82000022166.823559.1023570.1220210018874.518874.546087.81PROCESSED57614.16907407415713456768.72158564823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080074With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP8AO8SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
ETA CARINAE161.1825-59.711287.57247158-0.67238651329.300156476.182129629656479.0417361111408018010975241800009752497524097524220210087836.787836.7247049.72PROCESSED57611.7689120375686156492.72869212963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080081Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms.GALACTIC POINT SOURCES4BYUASATAKAYUKINULLNULLJAP8AO8DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAEHXDY
ETA CARINAE161.2758-59.6779287.59865979-0.62113788295.334356479.048043981556481.289050925940801802083968.518000083968.583968.5083968.5220210075778.675778.6193605.83PROCESSED57611.75482638895686156492.68673611113.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080081Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms.GALACTIC POINT SOURCES4BYUASATAKAYUKINULLNULLJAP8AO8DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAEXISY
V1223 SGR283.7562-31.1634.95737746-14.3520073175.000656745.629745370456746.500243055640801901029349.318000029389.329349.3029396.711021002613126131751921PROCESSED57614.14287037045712156756.75228009263.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080086A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS.GALACTIC POINT SOURCES4BYUASATAKAYUKINULLNULLJAP8AO8DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGRXISY
V1223 SGR283.7576-31.16294.95796111-14.3530681889.599256757.902361111156761.5211111111408019020150768.360000150776.3150776.30150768.32202100146315.8146315.8312605.73PROCESSED57614.32799768525715256789.79856481483.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080086A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS.GALACTIC POINT SOURCES4BYUASATAKAYUKINULLNULLJAP8AO8DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGRXISY
CXO J172641.7-354052261.6769-35.6761352.17176486-0.26901827279.452956540.00327546356540.801550925940802101037316.54000037331.737334.9037316.5230210035369.335369.368965.90PROCESSED57612.51120370375695656587.70635416673.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080100We propose an additional Suzaku observation of an unclassified gamma-ray source detected with the Fermi LAT telescope. In previous cycles, we found an enigmatic source XSS J12270-4859 to be the first gamma-ray binary among the low-mass X-ray binaries. This proposal aims to find a second source of the same nature for the most prospective target extracted from our catalogue search.GALACTIC POINT SOURCES4CTSUJIMOTOMASAHIRONULLNULLJAP8AO8X-RAY SEARCH OF ANOTHER ENIGMATIC SOURCE IN OUR GALAXYXISY
V2301 OPH270.15198.161234.5366484414.98247082262.070356573.987835648256576.000289351840802401040135.615000040135.640135.6040135.6220210065684.365684.3173858.71PROCESSED57612.90689814825718456596.57449074073.0.22.444Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080107It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.GALACTIC POINT SOURCES4AHAYASHITAKAYUKINULLNULLJAP8AO8MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLEXISY
V2301 OPH270.1558.156534.5336686714.97765204262.067956576.000300925956577.345231481540802402053188.411000053188.453188.4053188.4220210047289.247289.2116189.80PROCESSED57612.95833333335718456631.67542824073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080107It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.GALACTIC POINT SOURCES4AHAYASHITAKAYUKINULLNULLJAP8AO8MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLEXISY
V2301 OPH270.14378.176434.5471065714.9964302871.900856752.992280092656754.694594907440802403062925.35700062941.362925.3062941.3220210056503.756503.7147067.71PROCESSED57614.20916666675718456817.81498842593.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22080107It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion.GALACTIC POINT SOURCES4AHAYASHITAKAYUKINULLNULLJAP8AO8MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLEXISY
V1159 ORI82.2495-3.563206.52568579-19.93854352268.434856732.391585648256737.0939583333408029010200548.7200000200556.7200548.70200556.73202100188992.7188992.7404022.63PROCESSED57614.12019675935638356807.88677083333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081211We propose two 200 ks Suzaku observations of the dwarf nova V1159 Ori, chosen as our target because it is a known X-ray source with an extremely short (~4 day) outburst cycle. Each proposed observation will take ~5 calendar days and cover a complete outburst cycle. The dense X-ray coverage of the early rise in particular will be unprecedented for any dwarf nova, which is essential to further our understanding of the response of the boundary layer to the increased mass flux from the Keplerian accretion disk. We will also determine whether X-ray flux increases or decreases during quiescence to test the disk instability model. We will interpret the detailed picture of V1159 Ori in the context of existing, though less complete, X-ray campaigns on several other dwarf novae.GALACTIC POINT SOURCES4AMUKAIKOJINULLNULLUSA8AO8X-RAY EMISSION THROUGH COMPLETE OUTBURST CYCLES OF THE DWARF NOVA V1159 ORIXISY
SWIFT J2319.4+2619349.881926.247398.48369948-32.22425134253.996356633.879687556634.878611111140803001041275.84000041275.841275.8041275.81101100381493814986287.92PROCESSED57613.53693287045703956672.63005787043.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081213Polars are a subclass of magnetic cataclysmic variables in which a strongly magnetic white dwarf accretes matter from a late-type, Roche-lobe filling mass donor. They are usually soft X-ray bright and hard X-ray dim, due to either buried shocks or strong cyclotron cooling, depending on system parameters. However, a small subset of polars have been detected as bright hard X-ray sources in INTEGRAL and Swift BAT surveys. As a part of an effort to understand the hard-to-soft X-ray luminosity ratios of polars in general, and specifically to understand what combination of parameters make some polars hard X-ray bright, we propose Suzaku observations of two poorly studied BAT polars, Swift J2319.4+2619 and IW Eri, supported by ground-based observations including optical polarimetry.GALACTIC POINT SOURCES4CMUKAIKOJINULLNULLUSA8AO8THE HARD X-RAY BRIGHT POLARS SWIFT J2319.4+2619 AND IW ERIXISY
CD -28 3719105.2866-29.1168240.20191687-10.8915736697.072356577.359363425956579.41609953740803201014367.99000014367.990077.7090077.7320210078356.978356.9177665.91PROCESSED57645.49996527785700956642.76674768523.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081214Since they were discovered, it has been almost impossible to directly observe the accretion region in most symbiotic stars, in which a white dwarf (WD) accretes from the wind of a red giant. With the discovery that hard X-ray emission (E > 2 keV) is a common feature of WD symbiotics, that situation has finally changed. We propose to use Suzaku observations of 3 typical symbiotics with hard X-ray emission to test the hypothesis that such emission emanates from an accretion-disk boundary layer. With the proposed observations, we will determine whether the WD's magnetic field is high enough to disrupt the accretion flow, and estimate the WD mass and accretion rate. This work has implications for the study of accretion in wide binaries and symbiotics stars as progenitors of SNIa.GALACTIC POINT SOURCES4BSOKOLOSKIJENNIFERNULLNULLUSA8AO8X-RAYS FROM THE ACCRETION FLOWS IN SYMBIOTIC STARSXISY
SERPENS X-1279.99265.026536.110965984.83541867266.673256566.431203703756570.38217592594080330101760.52500009505.634855.301760.52202100130329.3130329.3341289.92PROCESSED57612.94810185185719856588.81820601853.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081222Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs.GALACTIC POINT SOURCES4BCACKETTEDWARDNULLNULLUSA8AO8THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIESXISY
SERPENS X-1279.98745.044536.124731154.8481741393.499756729.121527777856731.64596064824080330201215.41200006566.624077.201215.4220210082357.882357.8218087.94PROCESSED57614.0789120375719856747.8220370373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081222Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs.GALACTIC POINT SOURCES4BCACKETTEDWARDNULLNULLUSA8AO8THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIESXISY
SERPENS X-1279.98775.042436.122986634.8469585281.300956757.350706018556757.8959259259408033030388250001807.16459.50388330310023026.623026.647097.90PROCESSED57614.23314814825719856821.73524305563.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081222Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs.GALACTIC POINT SOURCES4BCACKETTEDWARDNULLNULLUSA8AO8THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIESXISY
GX 339-4255.7085-48.7866338.94274721-4.32598042275.400856526.572696759356529.3592476852408034010101019.6100000101019.6101019.60101019.6220210090316.990316.9240709.71PROCESSED57612.50836805565695656588.95900462963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22081242Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection bump.GALACTIC POINT SOURCES4ATOMSICKJOHNNULLNULLUSA8AO8-TOOCONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIESXISY
FS AURIGAE86.94528.5962180.536299660.2281128190.595556541.187905092656542.80297453740804101062184.26200062184.262184.2062184.2220210061028.761028.7139515.80PROCESSED57612.56758101855698156616.71650462963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22082012FS Aur represents one of the most unusual cataclysmic variable to have ever been observed. It is famous for a variety of uncommon and puzzling periodic photometric and spectroscopic variabilities. Tovmassian, Zharikov & Neustroev (2007) proposed that the precession of a fast-rotating magnetically accreting white dwarf can successfully explain these phenomena. We request 62 ks observations of FS Aur to detect the magnetic WD, determine its spin period, confirm the flux and spectral variability with the precession period, inconclusively detected by Chandra and Swift, and thus to check the proposed model. The theory of compact objects predicts certain relations between the spin and precession periods, and our findings will provide a good test for the theory.GALACTIC POINT SOURCES4BNEUSTROEVVITALYNULLNULLEUR8AO8PROBING THE PRECESSION OF WHITE DWARF IN CLOSE BINARY SYSTEMS - FS AURIGAEXISY
4U 1735-44264.7467-44.4484346.05710105-6.99533469268.998556917.784988425956918.998819444440804302010177.26000010177.210201.6010304.722020000000PROCESSED57616.55009259265762656940.62960648153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22082017We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated.GALACTIC POINT SOURCES4AEGRONELISENULLNULLEUR8AO8BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKUXISY
4U 1735-44264.7398-44.4536346.05003995-6.9938576996.437957098.691840277857099.27178240744080430304366.5200004366.54915.90496722020000000PROCESSED57617.82090277785747957112.4026620373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22082017We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated.GALACTIC POINT SOURCES4AEGRONELISENULLNULLEUR8AO8BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKUXISY
GRO J1008-57152.4313-58.2999282.99773034-1.83149103115.501256660.654814814856661.589756944440804401015337.42000015337.415347.9015337.4330310022179.422179.455037.91PROCESSED57613.73939814825704056679.76526620373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22082019We propose to observe the transient XRB GRO J1008&#8722;57 for 20 ks during an outburst in 2014 January after the currently ongoing giant outburst. The source exhibits regular outbursts once per orbit. Several of these outbursts have been observed in the past showing that the spectral shape remains constant between outbursts. Since we were able to improve the orbital ephemeris it is possible to predict future outbursts of the source. The source is currently (MJD 56245) exhibiting a giant type II outburst showing that the companion has ejected large amounts of material. We therefore propose to observe the system after this outburst to check for spectral and temporal changes and to study the iron line complex to derive the amount and ionization state of the material.GALACTIC POINT SOURCES4AKREYKENBOHMINGONULLNULLEUR8AO8MEASURING THE RESIDUAL MATERIAL IN GRO J1008&#8722;57 AFTER THE GIANT OUTBURSTXISY
X 1630-472248.5014-47.3935336.908464420.2525324288.631757073.237488425957074.41118055564090070106152.84000061656182.306152.833030000000PROCESSED57617.65700231485745457087.45730324073.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090015Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP9AO9-TOOMULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
X 1630-472248.5012-47.3939336.908078690.2523605588.632157077.062557870457078.11402777784090070205529.64000055475565.905529.622020000000PROCESSED57617.68792824075745457087.46052083333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090015Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP9AO9-TOOMULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
X 1630-472248.5011-47.3955336.906857210.2513248888.633457080.10312557081.15428240744090070305110.84000051285145.205110.811010000000PROCESSED57617.73936342595745857091.45795138893.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090015Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP9AO9-TOOMULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
H1743-322266.2607-32.2285357.12541364-1.6105206285.428856932.636562556933.28483796340900801015009.44000015601.215616.9015009.422020000000PROCESSED57616.60965277785734556979.40225694443.0.22.443Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090015Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP9AO9-TOOMULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
H1743-322266.5672-32.2343357.25542532-1.83494451273.377356939.733923611156940.524513888940900802019000.64000019000.619014.5019011.533030000000PROCESSED57616.63178240745734556979.4079745373.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090015Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition.GALACTIC POINT SOURCES4AUEDAYOSHIHIRONULLNULLJAP9AO9-TOOMULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURSTXISY
SAGITTARIUS A*266.4193-29.0102359.94333122-0.04924818267.302756929.144155092656929.666840277840901101020218.32000020218.320330.3020354.322020000000PROCESSED57616.58612268525674856979.40398148153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090048With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP9AO9SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4217-29.0078359.94647323-0.04978962278.801156938.087986111156938.461909722240901102017260.52000017260.517260.5017260.522020000000PROCESSED57616.62096064825674856979.40910879633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090048With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP9AO9SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.415-29.0097359.94179901-0.04577777105.770457095.319317129657096.495277777840901103025549.62000025549.647355.1047352.211010000000PROCESSED57617.79107638895674857111.3945254633.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090048With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP9AO9SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.415-29.0091359.94231116-0.0454652105.850257103.317453703757103.769016203740901104023242.22000023242.223246.5023246.511010000000PROCESSED57617.83428240745674857114.60784722223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090048With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP9AO9SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
SAGITTARIUS A*266.4146-29.0061359.94468967-0.04360372105.815957113.021516203757113.682766203740901105028670.62000028670.628670.6028686.622020000000PROCESSED57617.8917129635674857125.40087962963.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090048With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window.GALACTIC POINT SOURCES4AMAEDAYOSHITOMONULLNULLJAP9AO9SUZAKU MONITORING OF SGR A* GIGIANTIC FLAREXISY
1RXSJ171405.2-202747258.5195-20.45863.2194584110.6198626493.1857079.838402777857080.097465277840901201010977.71000010977.711001.7010993.711010000000PROCESSED57617.66413194445745857091.45878472223.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090051We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4BMORIHIDEYUKINULLNULLJAP9AO9SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ182853.8-241746277.2212-24.29328.76671438-6.1941437187.341957120.500509259357120.82174768524090130109707.2120009707.211842.2011850.232020000000PROCESSED57617.94474537045749657129.40741898153.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090051We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4BMORIHIDEYUKINULLNULLJAP9AO9SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ165739.1-294946254.4116-29.828353.327614088.1048004398.109757103.773333333357104.229432870440901401017225.51200017225.517257.5017233.511010000000PROCESSED57617.83942129635748657119.42114583333.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090051We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4BMORIHIDEYUKINULLNULLJAP9AO9SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ173916.2-214746264.8155-21.79125.333115684.9737732696.709757115.006006944457115.268171296340901501012328120001234912352.301232822020000000PROCESSED57617.89728009265749357126.4156253.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090051We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4BMORIHIDEYUKINULLNULLJAP9AO9SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ170856.9-235936257.2347-23.9931359.585273939.5684490895.208557099.276562557099.603032407440901601015376.81500015376.815384.8015376.811010000000PROCESSED57617.80537037045747957112.40721064823.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22090051We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe.GALACTIC POINT SOURCES4BMORIHIDEYUKINULLNULLJAP9AO9SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGEXISY
1RXSJ174559.6-370055266.4961-37.0139353.13065719-4.2608379995.253557115.272210648257115.665324074140901701014247.31500014247.314247.3014263.322020000000PROCESSED57617.90027777785749357126.41709490743.0.22.442Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V