te 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} : VS10a {Your family name} : Fomalont {Your given name} : Ed {The date you prepared this document (format is day-month-year, e.g 23-04-1999)} : 02-10-1999 {The name of the survey source that was observed} : J0842+18 {The name of the calibration source(s) observed} : 0808+019 {The year the experiment took place (e.g. 1998)} : 1999 {The starting day number of the experiment} : 8 {List the GRTs that observed} : HO, MP, SH {List the tracking stations that took part} : TZ {Which correlator was used to correlate the data? (Mitaka/Penticton/Socorro)} : Penticton {AIPS Version used (e.g 15OCT98)} : 15OCT99 {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} : No fringes were obtained from HALCA. They were not found at Penticton either. The three ground stations, HO, MP, SH seem to produce reasonable data. Some of the space baselines are short and the source should have been detected. \\ Suggest that this one be rescheduled. #--------------------------------------------------------------------------- # Section 2 : Pre-AIPS Checklist #--------------------------------------------------------------------------- {PI letter retrieved (yes/no)} : no {Data quality reports and plots retrieved? (yes/no)} : no {Pre-launch 5GHz survey data retrieved? (yes/no)} : yes {Light-curve data retrieved? (yes/no)} : no # Input files for INDXR, ANTAB and UVFLG {Has a INDXR input file (INDXR.TXT) been created? (yes/no)} : no {Has a ANTAB input file (ANTAB.TXT) been created? (yes/no)} : no {Has a UVFLG input file (UVFLG.TXT) been created? (yes/no)} : no {Any comments on Pre-AIPS file preparation?} : Very little flaging after Penticton apriori flagging needed. #--------------------------------------------------------------------------- # 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)} : no {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)} : no {IF 2 [SN_APCAL_2.PS] (yes/no)} : no # 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)} : 01 {Post-FRING CALIB SNPLT, Phase: IF 1 [SN_CALIB_PHA_1] (yes/no)} : no {IF 2 [SN_CALIB_PHA_2] (yes/no)} : no {Delay: IF 1 [SN_CALIB_DEL_1] (yes/no)} : no {IF 2 [SN_CALIB_DEL_2] (yes/no)} : no {Rate: IF 1 [SN_CALIB_RAT_1] (yes/no)} : no {IF 2 [SN_CALIB_RAT_2] (yes/no)} : no {SNR: IF 1 [SN_CALIB_SNR_1] (yes/no)} : no {IF 2 [SN_CALIB_SNR_2] (yes/no)} : no {Post-calibration VPLOT (amp and phase, with channel averaging) IF 1 [VPLOT_AP_1.PS] (yes/no)} : {IF 2 [VPLOT_AP_1.PS] (yes/no)} : {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)} : no {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), [J0842+18_FOMALONT_AIPS.FITS] (yes/no)} : yes [J0808+019_FOMALONT_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} : 0842.mod {Description} : VLBA modelfit to source. Compare with model.mod #--------------------------------------------------------- #--------------------------------------------------------------------------- # 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} :FRING {ADVERBs} : solint = 5 dparm = 2, 4000, 200, 0.5 {Input CL} : 1 {Input SN} : {Output SN} : 1 {Output CL} : {Comments} :No HALCA fringest obtained. See plots #--------------------------------------------------------- #--------------------------------------------------------- {Task} :SPLIT, UVAVG {ADVERBs} : {Input CL} : 1 {Input SN} : {Output SN} : {Output CL} : {Comments} : Average original data base to make 16ch, with 4-sec sampling. To be used with ground #--------------------------------------------------------- {Task} :FRING {ADVERBs} : solint = 5 dparm = 2, 1000, 50, 4 {Input CL} : 1 {Input SN} : {Output SN} : 1 {Output CL} : {Comments} :Fring of ground data only. #--------------------------------------------------------- #--------------------------------------------------------- {Task} :CLCOR {ADVERBs} : interp 'cube' dparm = 2, 1000, 50, 4 {Input CL} : 1 {Input SN} : 1 {Output SN} : {Output CL} : 2 {Comments} : Apply ground fring #--------------------------------------------------------- #--------------------------------------------------------- {Task} :CLCOR {ADVERBs} : ante 1,0 HO clcor = 66,0 ante 2,0 MP clcor = 33,0 ante 3,0 SH clcor = 66,0 ante 4,0 VSOP clcor = 120, 0 (just for completeness) {Input CL} : 3 {Input SN} : {Output SN} : 3 {Output CL} : {Comments} :These values chosen to make 0811+014 = 1.6 Jy. Model fut of ground data to J0842+18 with this calibration gives amplitudes a bit too high. See discussion at end of difmap section. #--------------------------------------------------------- #--------------------------------------------------------------------------- # Section 6 : Difmap data reduction notes #--------------------------------------------------------------------------- {Phase Selfcal applied? (yes/no)} : no {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)} : no {Comments on Difmap processing. Include the global amplitude offsets that were applied if gscal was used} : Diffmap was used to check on the ground data. The VLBA model fit from 1996 observations is in 0842.mod. The best model fit to this VSOP data, starting with the VLBA model, is given in model.mod. The major difference is that the flux density near the core was 0.8 Jy for the VLBA 1996 observations, but is now 1.1 Jy with the VSOP observations in 1999. There are no radio light curves available to see if the source was increasing in flux density. See vplots of data. #--------------------------------------------------------------------------- # Do not delete or alter anything past this line {VSOP Survey Checklist and Worksheet version} : 0.3 #---------------------------------------------------------------------------