# # 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} : VS09i {Your family name} : Paragi {Your given name} : Zsolt {The date you prepared this document (format is day-month-year, e.g 23-04-1999)} : 31-08-2001 {The name of the survey source that was observed} : J0824+5552 {The name of the calibration source(s) observed} : J0927+3902, J1800+7828 {The year the experiment took place (e.g. 1998)} : 2000 {The starting day number of the experiment} : 289 {List the GRTs that observed} : KASHIMA, NOTO, KALYAZIN {List the tracking stations that took part} : Usuda (UZ), Tidbinbilla (TZ) {Which correlator was used to correlate the data? (Mitaka/Penticton/Socorro)} : Mitaka {AIPS Version used (e.g 15OCT98)} : 31DEC01 {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} : There were difficulties with the calibration of Kalyazin. The residual fringe rate was huge (several hundreds of mHz) and highly variable (~60-80 mHz) on timescales of minutes. I had to fringe-fit Kalyazin with a solution interval of 15 seconds(!). This way I was able to recover the phases. An amplitude correction factor of 5 was also applied. The rest of the array was OK, FRING succeeded most of the time. An image was made in Difmap: slighlty resolved core. The source was a bit fainter than during the pre-launch VLBA observations. I had to modify the SURVEY run file for AIPS in order to produce non-standard outputs: FRING results for Kalyazin can be found in *FRING01* files while for the rest of the array in *CALIB* files. #--------------------------------------------------------------------------- # 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)} : n # 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)} : y {IF 2 [SN_ACCOR_2.PS] (yes/no)} : y {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)} : 1 {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)} : n {IF 2 [VPLOT_AP_1.PS] (yes/no)} : n {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} : douvcomp 1 digicor -1 delcorr -1 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : JUW24 (an ULTRA60 computer) in JIVE #--------------------------------------------------------- {Task} : INDXR {ADVERBs} : cparm = 0, 0, 0.1, 0 infile 'indxr.txt' {Input CL} : {Input SN} : {Output SN} : {Output CL} : 1 {Comments} : The 6 sec. CL interval time is needed to cope with the unstable fringe rates at Kalyazin. #--------------------------------------------------------- {Task} : ACCOR {ADVERBs} : solint 2 {Input CL} : {Input SN} : {Output SN} : 1 {Output CL} : {Comments} : Two minutes solution interval. This way we have only a few bad data points; by applying a longer solint a long timerange is affected by bad data. #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : opcode = 'cali' interpol = '2pt' {Input CL} : 1 {Input SN} : 1 {Output SN} : {Output CL} : 2 {Comments} : #--------------------------------------------------------- {Task} : ANTAB {ADVERBs} : tyver = 1 gcver = 1 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Tsys for Noto is taken from observation logs. Gaincurves and nominal tsys for other antennas are downloaded from VSOP WWW pages. #--------------------------------------------------------- {Task} : APCAL {ADVERBs} : tyver = 1 gcver = 1 {Input CL} : {Input SN} : {Output SN} : 2 {Output CL} : {Comments} : #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : opcode = 'cali' interpol = '2pt' {Input CL} : 2 {Input SN} : 2 {Output SN} : {Output CL} : 3 {Comments} : #--------------------------------------------------------- {Task} : TACOP {ADVERBs} : {Input CL} : 3 {Input SN} : {Output SN} : {Output CL} : 4 {Comments} : #--------------------------------------------------------- {Task} : TABED {ADVERBs} : optype 'add' aparm 19, 0, 0, 2, 4, 3 keyval -5E-11 0 {Input CL} : 4 {Input SN} : {Output SN} : {Output CL} : 4 {Comments} : Shift Kalyazin data in fring rate space by -5E10-11 sec/sec (reported from correlator). #--------------------------------------------------------- {Task} : FRING {ADVERBs} : antennas 1 3 refant = 1 solint = 0.25 aparm = 2, 0, 0, 0, 2, 1, 3 dparm = 3, 400, 1000, 0.5 {Input CL} : 4 {Input SN} : {Output SN} : 3 {Output CL} : {Comments} : There was a need to fringe-fit Kalyazin first with a very short solint. A high fringe rate window was necessary to do this. Fringes were found with good SNR. #--------------------------------------------------------- {Task} : FRING {ADVERBs} : antennas 1 2 4 5 refant = 1 search = 1, 2 solint = 3 aparm = 2, 0, 0, 0, 2, 1, 3, 0, 1 dparm = 3, 400, 100, 0.5 {Input CL} : 4 {Input SN} : {Output SN} : 4 {Output CL} : {Comments} : Fringe-fit for the rest of the array: OK. #--------------------------------------------------------- {Task} : TACOP {ADVERBs} : {Input CL} : 4 {Input SN} : {Output SN} : {Output CL} : 5 {Comments} : #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : opcode = 'cali' interpol = 'ambg' antennas 1 3 refant 1 {Input CL} : 4 {Input SN} : 3 {Output SN} : {Output CL} : 5 {Comments} : Apply solutions for Kalyazin. #--------------------------------------------------------- {Task} : CLCAL {ADVERBs} : opcode = 'cali' interpol = 'ambg' antennas 1 2 4 5 refant 1 {Input CL} : 4 {Input SN} : 4 {Output SN} : {Output CL} : 5 {Comments} : Apply solutions for the rest of the array. #--------------------------------------------------------- {Task} : POSSM {ADVERBs} : {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : {Comments} : Strong phase variations at the edges of the band in Noto data. Flag 10 channels in each sides of both IFs when splitting! #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : aparm = 2, 0.5, 0, 1 sources 'J0824+55' '' {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : {Comments} : Look at data in Difmap. Need to multiply Kalyazin amplitudes by a factor of five. Difmap does not understand MNTSTA=3 for HALCA. #--------------------------------------------------------- {Task} : TABED {ADVERBs} : aparm 5 0 0 2 4 4 keyval = 2 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Correct antenna type for VSOP_UZ (MNTSTA: orbiter->2) #--------------------------------------------------------- {Task} : TABED {ADVERBs} : aparm 5 0 0 2 4 5 keyval = 2 {Input CL} : {Input SN} : {Output SN} : {Output CL} : {Comments} : Correct antenna type for VSOP_TZ (MNTSTA: orbiter->2) #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : antennas 3 0 opcode 'gain' clcorprm 5 0 {Input CL} : 5 {Input SN} : {Output SN} : {Output CL} : 6 {Comments} : Multiply Kalyazin amplitudes by a factor of 5. #--------------------------------------------------------- {Task} : CLCOR {ADVERBs} : antennas 0 opcode 'gain' clcorprm 1.063 0 {Input CL} : 6 {Input SN} : {Output SN} : {Output CL} : 7 {Comments} : Correct for a factor of 1.13 Mitaka losses. See VSOP News No. 129, 25 May 2001. #--------------------------------------------------------- {Task} : SPLIT {ADVERBs} : aparm 2, 0.5, 0, 1 bchan 10 echan 118 {Input CL} : 7 {Input SN} : {Output SN} : {Output CL} : {Comments} : Split all sources. #--------------------------------------------------------- {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} : KALYAZIN {Amplitude correction factors} : 5.0 #--------------------------------------------------------------------------- # 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)} : y {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} : Compact, slightly resolved core. Amplitude correction factors are averages of IF1 and IF2 corrections; there were no significant differences between IF1 and IF2 factors. # 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} : KASH NOTO KALY UZ TZ {Amplitude correction factors} : 1.02 1.07 1.03 0.92 0.93 #--------------------------------------------------------------------------- # Do not delete or alter anything past this line {VSOP Survey Checklist and Worksheet version} : 0.4 #---------------------------------------------------------------------------