# # Template Checklist and Worksheet for reduction of VSOP Survey data. # (http://halca.vsop.isas.ac.jp/survey/template_checklist.txt) # # Version 0.4 - J. Lovell 6-October-1999 # - added amplitude correction factor entries # Version 0.3 - J. Lovell 14-Apr-1999 # # NOTE: Copy this file to your data reduction outputs directory (e.g # /something/vs05a_jones) and name it "checklist.txt" # # Comments are given on lines beginning with a # and questions are # enclosed in {}'s. # Please enter responses after the colons. # Multiple-line responses are OK. # Yes/No questions may be answered with "yes", "no", "Y", "N", "y" or "n" # An example of a completed Checklist is given in # http://halca.vsop.isas.ac.jp/survey/checklist_eg.txt # # #--------------------------------------------------------------------------- # Section 1 : General Information #--------------------------------------------------------------------------- {Experiment code} : VS02v {Your family name} : Scott {Your given name} : William {The date you prepared this document (format is day-month-year, e.g 23-04-1999)} : 24-02-2000 {The name of the survey source that was observed} : J1107-44 {The name of the calibration source(s) observed} : J1127-18 {The year the experiment took place (e.g. 1998)} : 1999 {The starting day number of the experiment} : 147 {List the GRTs that observed} : AT, Ho, Se {List the tracking stations that took part} : UZ, RZ {Which correlator was used to correlate the data? (Mitaka/Penticton/Socorro)} : Penticton {AIPS Version used (e.g 15OCT98)} : 15Apr99 {Difmap Version used (e.g 2.3c)} : 2.3c {Was vsop_difmap used? (yes/no)} : y {Abstract. Write a brief summary of the data reduction and its outcomes} : #--------------------------------------------------------------------------- # Section 2 : Pre-AIPS Checklist #--------------------------------------------------------------------------- {PI letter retrieved (yes/no)} : y {Data quality reports and plots retrieved? (yes/no)} : y {Pre-launch 5GHz survey data retrieved? (yes/no)} : n {Light-curve data retrieved? (yes/no)} : y # Input files for INDXR, ANTAB and UVFLG {Has a INDXR input file (INDXR.TXT) been created? (yes/no)} : y {Has a ANTAB input file (ANTAB.TXT) been created? (yes/no)} : y {Has a UVFLG input file (UVFLG.TXT) been created? (yes/no)} : n {Any comments on Pre-AIPS file preparation?} : #--------------------------------------------------------------------------- # Section 3 : AIPS Output File Checklist # # Names of expected output file names are contained in square brackets. #--------------------------------------------------------------------------- {PRTAN [PRTAN.LIS] (yes/no)} : yes {LISTR (optyp = 'SCAN') [LISTR.LIS] (yes/no)} : yes {DTSUM (aparm = 0) [DTSUM_0.LIS] (yes/no)} : yes {DTSUM (aparm = 1) [DTSUM_1.LIS] (yes/no)} : yes {UVPLT (u vs v) [UVPLT_UV.PS] (yes/no)} : yes {UVPLT ((u,v) distance vs time) [UVPLT_UVD.PS] (yes/no)} : yes {UVPLT ((u,v) position angle vs time). [UVPLT_UVPA.PS] (yes/no)} : yes {VPLOT antenna weights vs time (after adjustment) [WEIGHTS.PS] (yes/no)} : yes {ACCOR SNPLT (amplitude), IF 1 [SN_ACCOR_1.PS] (yes/no)} : no {IF 2 [SN_ACCOR_2.PS] (yes/no)} : no {APCAL SNPLT (amplitude), IF 1 [SN_APCAL_1.PS] (yes/no)} : yes {IF 2 [SN_APCAL_2.PS] (yes/no)} : yes # FRING SNPLT (delay, rate, SNR), as many as necessary to document the # clear discovery of fringes at all antennas, numbered with "nn" for # both IFs. Do NOT include the final SN table as it is plotted later. # # Format is SN_FRINGnn_DEL_i.PS, SN_FRINGnn_RAT_i.PS, # SN_FRINGnn_SNR_i.PS for delay, rate and SNR plots respectively, # where "i" is the IF number (1 or 2). {Number of times preliminary FRING solutions were plotted (i.e maximum value of nn)} : 0 {Post-FRING CALIB SNPLT, Phase: IF 1 [SN_CALIB_PHA_1] (yes/no)} : yes {IF 2 [SN_CALIB_PHA_2] (yes/no)} : yes {Delay: IF 1 [SN_CALIB_DEL_1] (yes/no)} : yes {IF 2 [SN_CALIB_DEL_2] (yes/no)} : yes {Rate: IF 1 [SN_CALIB_RAT_1] (yes/no)} : yes {IF 2 [SN_CALIB_RAT_2] (yes/no)} : yes {SNR: IF 1 [SN_CALIB_SNR_1] (yes/no)} : yes {IF 2 [SN_CALIB_SNR_2] (yes/no)} : yes {Post-calibration VPLOT (amp and phase, with channel averaging) IF 1 [VPLOT_AP_1.PS] (yes/no)} : yes {IF 2 [VPLOT_AP_1.PS] (yes/no)} : yes {Post-calibration POSSM (amplitude and phase, at least one 5 to 10 min integration spectrum per tracking pass, indexed with nn = 01, 02, 03, ...), IF 1 [POSSMnn_AP_1.PS] (yes/no)} : yes {IF 2 [POSSMnn_AP_2.PS] (yes/no)} : no {Output TASAV FITS file (containing all 'multisource' cal tables) [VSxxx__TASAV.FITS] (yes/no)} : yes {Calibrated and spectrally averaged FITS data files (one for each source), [__AIPS.FITS] (yes/no)} : yes #--------------------------------------------------------------------------- # Section 4 : Supplementary files # # Were any files created, other than those listed, to document the data # reduction? If so, please list them below using as many (File, Description) # groups as required. #--------------------------------------------------------------------------- #------------------------------------------------------------------------- # Section 5 : AIPS data-reduction notes # # The format is as follows: # # Task : the name of the task that is run or other operation performed # ADVERBs : a list of the relevant non-default adverbs # Input CL : the input calibration table used (if any) in running the task # Input SN : the SN table that was used (if any) # Output SN : the SN table produced (if any) # Output CL : the CL table produced or modified (if any) # Comments: any comments on the results of the operation # # Use as many of the (Task, ADVERBs, Comments, Input CL, Input SN, # Output SN, Output CL) groups as required. #------------------------------------------------------------------------- #--------------------------------------------------------- {Task} : FITLD {ADVERBs} : DIGICOR=DELCOR=-1 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Output file name = VS02v.FITLD #--------------------------------------------------------- #--------------------------------------------------------- {Task} : MSORT {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Input file name = VS02v.FITLD, Output file name = VS02v.UVSRT #--------------------------------------------------------- #--------------------------------------------------------- {Task} : INDXR {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Created NX(1) #--------------------------------------------------------- #--------------------------------------------------------- {Task} : ANTAB {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Used Tsys values of 92,96K for Halca. For the AT, used nominal values (as far as I could tell, all 6 telescopes observed). For Ho, assumed that the "tsys"'s in the tsys file were actually SEFDs. Output sent to TY(1) and GC(1). #--------------------------------------------------------- #--------------------------------------------------------- {Task} : APCAL {ADVERBs} : {Input CL} : {Input SN} : 1 {Output SN} : {Output CL} : {Comments} : Input: Ty(1) + GC(1) #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : OPCODE = CALP INTERPOL = 'AMBG' REFANT 1 (AT) {Input CL} : 1 {Input SN} : 1 {Output SN} : {Output CL} : 2 {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : TBOUT {ADVERBs} : INEXT = 'AN' {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : TBIN {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Changed MNTSTA entries in the AN table. Changed Halca from 3 to 2, changed Hobart from 2 to 0, and change Hart from 1 to 0 (although the latter change is irrelevant, since there was no Hart data). #--------------------------------------------------------- #--------------------------------------------------------- {Task} : TBIN {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : 2 {Output CL} : {Comments} : Read in DQA1 delay and rate solutions. #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : OPCODE = CALP INTERPOL = 'AMBG' REFANT 1 (AT) {Input CL} : 2 {Input SN} : 2 {Output SN} : {Output CL} : 3 {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : FRING {ADVERBs} : DOCALIB 1 GAINUSE 3 REFANT 1 (AT) SEARCH 4,5 SOLINT 3 APARM(1)=2 APARM(7)=2 (SNR=2) APARM(9)=1 DPARM(1)=3 (include baseline stacking) DPARM(2)=100 (100ns delay window!) DPARM(3)=50 (50mHz rate window) DPARM(4)=0.5 (0.5 sec integration time) DPARM(6)=1 (don't average in frequency) BCHAN 0, ECHAN 0 TIMER 0 11 0 0 to 0 11 30 0, then TIMER 0 13 0 0 to o 13 30 0 {Input CL} : 3 {Input SN} : {Output SN} : 3 {Output CL} : {Comments} : Got good solutions for all antennas, although Halca solutions were a little rattier during the TIMER starting at 0 13 0 0. Rate solutions were very small...so can reduce rate window more. Can reduce the delay window slightly as well to get more SNR. Will increase the solint to 4 to try to get more consistency in the Halca solns. #--------------------------------------------------------- #--------------------------------------------------------- {Task} : FRING {ADVERBs} : as above, except: SOLINT 4 DPARM(2)=60 (60ns delay window!) DPARM(3)=20 (20mHz rate window) TIMER 0 {Input CL} : 3 {Input SN} : {Output SN} : 3 (nuked old test SN table 3s) {Output CL} : {Comments} : Solutions looked great. #--------------------------------------------------------- #--------------------------------------------------------- {Task} : SNEDT {ADVERBs} : {Input CL} : {Input SN} : 3 {Output SN} : 4 {Output CL} : {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : OPCODE='CALP' INTERPOL = 'AMBG' SMOTYPE = '' REFANT 1 {Input CL} : 3 {Input SN} : 4 {Output SN} : {Output CL} : 4 {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : TACOP {ADVERBs} : {Input CL} : 4 {Input SN} : {Output SN} : {Output CL} : 5 {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : OPCODE = 'GAIN' ANTENNAS = 5 (Ho) CLCORPRM = 1.25 {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : 5 {Comments} : Compared near-crossing points. Compared UV points for Se-Ho at 12:58 and Se-Halca at 11:10. Assuming Halca calibration is ok, need to multiply Ho by 1.25 to obtain similar amplitudes. Similarly, compared the Halca-AT and Halca-Ho UV tracks. The latter UV tracks are lower by about 1.25. After applying this correction, now Se seems a little lowish compared to the other data, but I'll let amp self-cal take care of this. #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : OPCODE = 'GAIN' ANTENNAS = 0 CLCORPRM = 1.34 {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : 5 {Comments} : Using the calibrator source J1127-18 to try to establish an absolute amplitude scale proved fruitless. The source appeared highly variable (by about a factor of 2) at 8GHz over the timespan of a year, while the 2 GHz flux remained constant. For both 2 and 8 GHz, there were no observations within a year of the Halca observations. No AT light curves were available for the calibrator. The PLS data for the calibrator was about 3 years old. All of these observations of the calibrator were within the ballpark of the Halca radplot. For the target source, the only data I could find was the AT light curve. The last data point was over a year ago. However, J1107-44 appeared reasonably constant before that. Need to multiply the zero spacing flux by 1.8 to coincide with the AT data (even after the Ho correction). Multiply all antennas by 1.8**0.5, since other than this scaling factor (and the minor Ho correction), all the data in the radplot looked self-consistent. #--------------------------------------------------------- #--------------------------------------------------------- {Task} : TACOP {ADVERBs} : {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : 6 {Comments} : #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : OPCODE = 'GAIN' ANTENNAS = see below CLCORPRM = see below {Input CL} : 6 {Input SN} : {Output SN} : {Output CL} : 6 {Comments} : Applied the corrections I got from Difmap with gscale. If I let Difmap apply these corrections, I lose some of the data due to not having 4 co-observing antennas (even though gscale applies a GLOBAL amplitude scaling! Corrections were: IF1: AT 0.92, Sh 1.06, Ho 0.87, Halca 0.98 IF2: AT 0.92, Sh 1.13, Ho 0.88, Halca 1.12 #--------------------------------------------------------- #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : OPCODE = 'GAIN' ANTENNAS = 0 CLCORPRM = 1.08 {Input CL} : 6 {Input SN} : {Output SN} : {Output CL} : 6 {Comments} : When cleaning the (post initial CLCORed) data in Difmap, I could not clean out enough small spacing flux, without making the clean component model fits to the rest of the visibilites bad. Hence, I ran gscale anyhow (allowing the low-spacing flux to be dragged down), then compensated with CLCOR by multiplying all visibilities by 1.08**2 ~ 1.17. #--------------------------------------------------------- #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : SOURCES 'J1107-44','J1127-18' BCHAN 0, ECHAN 0 DOCALIB 1 GAINUSE 4 APARM(1)=2 (average each IF separately) APARM(2)=0.5 APARM(4)=1 {Input CL} : 4 {Input SN} : {Output SN} : {Output CL} : {Comments} : Input file: VS02V.UVSRT, Output files: J1107-44.noCLCO, J1127-18.FITS #--------------------------------------------------------- #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : SOURCES 'J1107-44' BCHAN 0, ECHAN 0 DOCALIB 1 GAINUSE 5 APARM(1)=2 (average each IF separately) APARM(2)=0.5 APARM(4)=1 {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : {Comments} : Input file: VS02V.UVSRT, Output files: J1107-44.CLCOR1 #--------------------------------------------------------- #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : SOURCES 'J1107-44' BCHAN 0, ECHAN 0 DOCALIB 1 GAINUSE 6 APARM(1)=2 (average each IF separately) APARM(2)=0.5 APARM(4)=1 {Input CL} : 6 {Input SN} : {Output SN} : {Output CL} : {Comments} : Input file: VS02V.UVSRT, Output files: J1107-44.CLCOR2 #--------------------------------------------------------- #--------------------------------------------------------- {Task} : FITTP {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Input files: J1107-44.noCLCO, J1127-18.FITS Output files: J1107-44.noCLCOR.FITS, J1127-18.noCLCOR.FITS #--------------------------------------------------------- #--------------------------------------------------------- {Task} : FITTP {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Input files: J1107-44.CLCOR1 Output files: J1107-44.CLCOR1.FITS #--------------------------------------------------------- #--------------------------------------------------------- {Task} : FITTP {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Input files: J1107-44.CLCOR2 Output files: J1107-44.CLCOR2.FITS #--------------------------------------------------------- #------------------------------------------------------------------------- # Section 6 : Antenna-based amplitude corrections #------------------------------------------------------------------------- # Corrections applied with CLCOR in AIPS to correct for antenna-based amplitude # errors. # Separate antenna names and correction factors by commas or spaces. # e.g # # {Antenna name list} : HALCA, HO, HH, MP, KA # {Amplitude correction factors} : 1.0, 1.6, 1.3, 1.0, 1.0 # {Antenna name list} : HALCA, AT, Ho, Se {Amplitude correction factors} : 1.33, 1.59, 1.57, 1.52 #------------------------------------------------------------------------- # Section 7 : Difmap data reduction notes #------------------------------------------------------------------------- {Phase Selfcal applied? (yes/no)} : y {Global Amplitude Selfcal applied? (yes/no)} : n {Amplitude Selfcal applied on non-global timescales? (yes/no)} : n {Modelfit made and saved using the vs_final_mod macro? (yes/no)} : y {Image made and saved using the vs_final_img macro? (yes/no)} : y {Comments on Difmap processing. Include the global amplitude offsets that were applied if gscal was used} : Imaged the source once, then model-fit the core to an elliptical Gaussian. Then, used this as a starting model for a second round of clean/self-cal. Used phase-self-cal down to a solint of 2 minutes. Did not run gscale, since these correction factors were already applied with CLCOR. Final image is resolved, with additional non-core components to the North and South-west. # If GSCAL was used, report amplitude correction factors here. If GSCAL # was used more than once, report the CUMULATIVE factor here (e.g if gscal # reported a gain factor of 1.11 for HALCA the first time and 0.95 the # second time, the overall gain correction is 1.11 * 0.95 = 1.05. # Separate antenna names and correction factors by commas or spaces. # e.g # # {Antenna name list} : HALCA, HO, HH, MP, KA # {Amplitude correction factors} : 1.0, 1.6, 1.3, 1.0, 1.0 # {Antenna name list} : {Amplitude correction factors} : #------------------------------------------------------------------------- # Do not delete or alter anything past this line {VSOP Survey Checklist and Worksheet version} : 0.4 #-------------------------------------------------------------------------