# # 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} : VS07t {Your family name} : Piner {Your given name} : Glenn {The date you prepared this document (format is day-month-year, e.g 23-04-1999)} : 02-11-1999 {The name of the survey source that was observed} : J0115-01 {The name of the calibration source(s) observed} : 0202+149 {The year the experiment took place (e.g. 1998)} : 1999 {The starting day number of the experiment} : 222 {List the GRTs that observed} : MP, HO, SH {List the tracking stations that took part} : GZ, TZ, RZ {Which correlator was used to correlate the data? (Mitaka/Penticton/Socorro)} : Penticton {AIPS Version used (e.g 15OCT98)} : 31DEC99 {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} : Found fringes to HALCA throughout the experiment using standard parameters in FRING. There was a delay jump of 200-300 nsec between the TZ and GZ tracking pass. Imaging this source was rather difficult. After cleaning the central region there was still considerable flux missing from the short baselines and a number of nearly equally bright residuals. Windowed the two brightest residuals, which also happen to be in the jet direction seen in the USNO image (if the northwest component is the core). Also did several iterations with natural weighting to more closely approach the short baseline flux. A 3-component circular model was fit to the data. The total flux density was only about 0.5 Jy, compared to 0.9 Jy from the AT light curve. #--------------------------------------------------------------------------- # 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)} : y {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)} : y {LISTR (optyp = 'SCAN') [LISTR.LIS] (yes/no)} : y {DTSUM (aparm = 0) [DTSUM_0.LIS] (yes/no)} : y {DTSUM (aparm = 1) [DTSUM_1.LIS] (yes/no)} : y {UVPLT (u vs v) [UVPLT_UV.PS] (yes/no)} : y {UVPLT ((u,v) distance vs time) [UVPLT_UVD.PS] (yes/no)} : y {UVPLT ((u,v) position angle vs time). [UVPLT_UVPA.PS] (yes/no)} : y {VPLOT antenna weights vs time (after adjustment) [WEIGHTS.PS] (yes/no)} : n {ACCOR SNPLT (amplitude), IF 1 [SN_ACCOR_1.PS] (yes/no)} : n {IF 2 [SN_ACCOR_2.PS] (yes/no)} : n {APCAL SNPLT (amplitude), IF 1 [SN_APCAL_1.PS] (yes/no)} : y {IF 2 [SN_APCAL_2.PS] (yes/no)} : y # 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)} : y {IF 2 [SN_CALIB_PHA_2] (yes/no)} : y {Delay: IF 1 [SN_CALIB_DEL_1] (yes/no)} : y {IF 2 [SN_CALIB_DEL_2] (yes/no)} : y {Rate: IF 1 [SN_CALIB_RAT_1] (yes/no)} : y {IF 2 [SN_CALIB_RAT_2] (yes/no)} : y {SNR: IF 1 [SN_CALIB_SNR_1] (yes/no)} : y {IF 2 [SN_CALIB_SNR_2] (yes/no)} : y {Post-calibration VPLOT (amp and phase, with channel averaging) IF 1 [VPLOT_AP_1.PS] (yes/no)} : y {IF 2 [VPLOT_AP_1.PS] (yes/no)} : y {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)} : y {IF 2 [POSSMnn_AP_2.PS] (yes/no)} : y {Output TASAV FITS file (containing all 'multisource' cal tables) [VSxxx__TASAV.FITS] (yes/no)} : y {Calibrated and spectrally averaged FITS data files (one for each source), [__AIPS.FITS] (yes/no)} : y #--------------------------------------------------------------------------- # 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} : infi 'VS07T_36CH.FITS' digicor = -1 delcorr = -1 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : loaded spectrally averaged file from Horiuchi Shinji #--------------------------------------------------------- {Task} : ANTAB {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : used ANTAB.TXT file from vs07t whiteboard #--------------------------------------------------------- {Task} : APCAL {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : 1 {Output CL} : {Comments} : #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : interpol '2pt' {Input CL} : 1 {Input SN} : 1 {Output SN} : {Output CL} : 2 {Comments} : Amplitude calibration solutions applied #--------------------------------------------------------- {Task} : FRING {ADVERBs} : docalib = 1 gainuse = 2 refant = 2 search = 3,4,1 solint = 10 aparm = 2,0,0,0,0,1,1,0,1,0 dparm = 0,1000,200,0,0 {Input CL} : {Input SN} : {Output SN} :2 {Output CL} : {Comments} :Fringes found with standard settings. Only a few missing fringes. Rerun with smaller rate window to see if detections improved. #--------------------------------------------------------- {Task} : FRING {ADVERBs} : docalib = 1 gainuse = 2 refant = 2 search = 3,4,1 solint = 10 aparm = 2,0,0,0,0,1,1,0,1,0 dparm = 0,1000,100,0,0 {Input CL} : {Input SN} : {Output SN} :3 {Output CL} : {Comments} : #--------------------------------------------------------- {Task} : TBOUT {ADVERBs} : {Input CL} : {Input SN} :3 {Output SN} : {Output CL} : {Comments} :write out SN table for editing with snedit.pl #--------------------------------------------------------- {Task} : TBIN {ADVERBs} : {Input CL} : {Input SN} : {Output SN} :4 {Output CL} : {Comments} :read in edited SN table #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : interpol 'ambg' refant=2 {Input CL} : 2 {Input SN} : 4 {Output SN} : {Output CL} : 3 {Comments} : #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : docalib=1 aparm=2,0 {Input CL} : 3 {Input SN} : {Output SN} : {Output CL} : {Comments} : #--------------------------------------------------------- {Task} : FITTP {ADVERBs} : {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Data written out for analysis in Difmap #--------------------------------------------------------- #--------------------------------------------------------------------------- # 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} : {Amplitude correction factors} : #--------------------------------------------------------------------------- # Section 7 : Difmap data reduction notes #--------------------------------------------------------------------------- {Phase Selfcal applied? (yes/no)} : y {Global Amplitude Selfcal applied? (yes/no)} : y {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} : Imaging this source was rather difficult. After cleaning the central region there was still considerable flux missing from the short baselines and a number of nearly equally bright residuals. Windowed the two brightest residuals, which also happen to be in the jet direction seen in the USNO image (if the northwest component is the core). Also did several iterations with natural weighting to more closely approach the short baseline flux. A 3-component circular model was fit to the data. The total flux density was only about 0.5 Jy, compared to 0.9 Jy from the AT light curve. # 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} : VSOP_SC, MOP, SESHAN25, HOBART, X {Amplitude correction factors} : 1.04, 0.86, 1.11, 0.96, X #--------------------------------------------------------------------------- # Do not delete or alter anything past this line {VSOP Survey Checklist and Worksheet version} : 0.4 #---------------------------------------------------------------------------