# # Template Checklist and Worksheet for reduction of VSOP Survey data. # (http://halca.vsop.isas.ac.jp/survey/template_checklist.txt) # # 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} : VS04t {Your family name} : Shen {Your given name} : Zhi-Qiang {The date you prepared this document (format is day-month-year, e.g 23-04-1999)} : 01-11-1999 {The name of the survey source that was observed} : J2329-47 {The name of the calibration source(s) observed} : 2255-282 {The year the experiment took place (e.g. 1998)} : 1998 {The starting day number of the experiment} : 170 {List the GRTs that observed} : HartRAO, Mop {List the tracking stations that took part} : RZ,UZ {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)} : yes {Abstract. Write a brief summary of the data reduction and its outcomes} : This is a 2 GRTs VSOP survey experiment. Good fringes were found to Halca during RZ pass as well as to two ground antennas all the time. Very weak fringes were seen during the 1 hr UZ pass, consistent with the DQA report. The uv-crossing points between two space baselines showed that the relative gains between two ground telescopes are good. If Halca is assumed to be okay, the whole amplitude scale is reasonable. This is also consistent with the fringes amplitude for the calibrator source (see below). Both imaging and model fitting went very well. A single circular Gaussian component model was used to fit the calibrated data. Strong fringes were detected for the calibrator (2255-282) on the ground baseline (HartRAO --- Mop) of 9,000km with a correlated flux density of 2.1Jy, quite consistent with the PLS results of 2.2Jy at about 7,200km. #--------------------------------------------------------------------------- # Section 2 : Pre-AIPS Checklist #--------------------------------------------------------------------------- {PI letter retrieved (yes/no)} : yes {Data quality reports and plots retrieved? (yes/no)} : yes {Pre-launch 5GHz survey data retrieved? (yes/no)} : no {Light-curve data retrieved? (yes/no)} : yes # Input files for INDXR, ANTAB and UVFLG {Has a INDXR input file (INDXR.TXT) been created? (yes/no)} : yes {Has a ANTAB input file (ANTAB.TXT) been created? (yes/no)} : yes {Has a UVFLG input file (UVFLG.TXT) been created? (yes/no)} : no {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)} : no {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)} : 1 {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)} : yes {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. #--------------------------------------------------------------------------- #--------------------------------------------------------- {File} : {Description} : #--------------------------------------------------------- #--------------------------------------------------------------------------- # 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} : douvcomp=1;dotable=1 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : load the uv FITS data into AIPS #--------------------------------------------------------- {Task} : MSORT {ADVERBs} : sort='TB' {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : sort the data to 'TB' order #--------------------------------------------------------- {Task} : INDXR {ADVERBs} : cparm(3)=1 {Input CL} : {Input SN} : {Output SN} : {Output CL} : 1 {Comments} : index uv data with 1 min CL entry interval #--------------------------------------------------------- {Task} : TACOP {ADVERBs} : {Input CL} : 1 {Input SN} : {Output SN} : {Output CL} : 2 {Comments} : protect original CL1 #--------------------------------------------------------- {Task} : ANTAB {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : determine the Tsys and gain curve (see ANTAB.TXT file). Tsys=95K for Halca #--------------------------------------------------------- {Task} : APCAL {ADVERBs} : opcode=' ' {Input CL} : {Input SN} : {Output SN} : 1 {Output CL} : {Comments} : generate an amplitude calibration solution table #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : opcode='CALI' smotype='ampl ' refant=0 {Input CL} : 2 {Input SN} : 1 {Output SN} : {Output CL} : 3 {Comments} : apply amplitude calibration solution #--------------------------------------------------------- {Task} : FRING {ADVERBs} : docalib=1 flagv=-1;solint=4;refant=1 aparm=2,0,0,0,0,1,2,0 dparm=1,0 antwt=1,1,30 {Input CL} : 3 {Input SN} : {Output SN} : 3 {Output CL} : {Comments} : FFT fringe fitting test run #--------------------------------------------------------- {Task} : TACOP {ADVERBs} : {Input CL} : 3 {Input SN} : {Output SN} : {Output CL} : 4 {Comments} : protect CL3 #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : opcode='sbdl';timer=0 antenna=2,0;clcorprm=-192.7,-192.7,0 (antenna=3,0;clcorprm=2143.2.,2143.2,0) {Input CL} : 4 {Input SN} : {Output SN} : {Output CL} : 4 {Comments} : apply delay offsets to each IF residual delay #--------------------------------------------------------- {Task} : FRING {ADVERBs} : docalib=1 flagv=-1;solint=4;refant=1 search=2,0 aparm=2,0,0,0,0,1,2,0,1,0 dparm=1,100,50,0 {Input CL} : 4 {Input SN} : {Output SN} : 13 {Output CL} : {Comments} : FFT+LLS fringe fitting with narrow searching windows #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : opcode='CALP';interpol='AMBG';smotype='VLBI' refant=1 cals=sour='J2329-47' (cals=sour='2255-282') {Input CL} : 4 {Input SN} : 13 {Output SN} : {Output CL} : 5 {Comments} : apply fringe fitting solutions (2 times) #--------------------------------------------------------- {Task} : TASAV {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : copy all extension tables to a dummy file #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : docalib=1;flagv=-1 douvcomp=1;aparm=2,0 {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : {Comments} : make calibrated single-source data files: J2329-47.SPLIT and 2255-282.SPLIT #--------------------------------------------------------- {Task} : FITTP {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : export each single-source file in FITS format to disk file for further imaging analysis #--------------------------------------------------------- #--------------------------------------------------------------------------- # Section 6 : Difmap data reduction notes #--------------------------------------------------------------------------- {Phase Selfcal applied? (yes/no)} : yes {Global Amplitude Selfcal applied? (yes/no)} : no {Amplitude Selfcal applied on non-global timescales? (yes/no)} : no {Modelfit made and saved using the vs_final_mod macro? (yes/no)} : yes {Image made and saved using the vs_final_img macro? (yes/no)} : yes {Comments on Difmap processing. Include the global amplitude offsets that were applied if gscal was used} : average data over 30 sec (uvaver 30,true) raise the weight of HALCA (selfant VSOP_SC,false,30) keep non-closing data during phase self-cal (selfflag false,3,4) clean and phase self-cal with uniform weighting (uvw 2,-1 ... etc) switch to natural weighting to clean more flux (uvw 0,-1 ... etc) switch back to obtain a uniform weighting clean image: peak=0.239 Jy/beam, RMS=7.7 mJy/beam; beam=0.545 mas x 0.244 mas @ 70.3 deg A circular Gaussian component model was fit the calibrated data. Calibrator (2255-282) was observed for 15 minutes by ground telescopes (HartRAO and Mop), and fringes were strong on the 9,000km ground baseline with a correlated flux density of 2.1Jy, quite consistent with the PLS results of 2.2Jy at about 7,200km. #--------------------------------------------------------------------------- # Do not delete or alter anything past this line {VSOP Survey Checklist and Worksheet version} : 0.3 #---------------------------------------------------------------------------