; UVHOL ;--------------------------------------------------------------- ;! prints holography data from a UV data base with calibration ;# TASK UV HARDCOPY CALIBRATION ;----------------------------------------------------------------------- ;; Copyright (C) 1999-2000, 2003 ;; Associated Universities, Inc. Washington DC, USA. ;; ;; This program is free software; you can redistribute it and/or ;; modify it under the terms of the GNU General Public License as ;; published by the Free Software Foundation; either version 2 of ;; the License, or (at your option) any later version. ;; ;; This program is distributed in the hope that it will be useful, ;; but WITHOUT ANY WARRANTY; without even the implied warranty of ;; MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the ;; GNU General Public License for more details. ;; ;; You should have received a copy of the GNU General Public ;; License along with this program; if not, write to the Free ;; Software Foundation, Inc., 675 Massachusetts Ave, Cambridge, ;; MA 02139, USA. ;; ;; Correspondence concerning AIPS should be addressed as follows: ;; Internet email: aipsmail@nrao.edu. ;; Postal address: AIPS Project Office ;; National Radio Astronomy Observatory ;; 520 Edgemont Road ;; Charlottesville, VA 22903-2475 USA ;----------------------------------------------------------------------- UVHOL LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC UVHOL Prints/writes holography data with calibration USERID -32000.0 32000.0 Data base owner number INNAME Input UV file name (name) INCLASS Input UV file name (class) INSEQ 0.0 9999.0 Input UV file name (seq. #) INDISK Input UV file disk unit # SOURCES Sources to print, ' '=>all. QUAL -10.0 Qualifier -1=>all CALCODE Calibrator code ' '=>all STOKES 'FULL' in HOLG for 4 output files, 'IQUV', 'IV' also SELBAND Bandwidth to select (kHz) SELFREQ Frequency to select (MHz) FREQID Freq. ID to select. TIMERANG Time range to select ANTENNAS Antennas to print BASELINE Baselines with ANTENNAS UVRANGE UV range in kilolambda. SUBARRAY 0.0 1000.0 Subarray, 0 => 1 CHANNEL 0.0 4096.0 Spectral channel # BIF IF number to print DOCALIB -1.0 2.0 If >0 calibrate data = 2 calibrate weights GAINUSE CAL (CL or SN) table to apply DOPOL -1.0 10.0 If >0 correct polarization. BLVER BL table to apply. FLAGVER Flag table version DOBAND -1.0 10.0 If >0 apply bandpass cal. Method used depends on value of DOBAND (see HELP file). BPVER Bandpass table version SMOOTH Smoothing function. See HELP SMOOTH for details. BCOUNT 0.0 9999999. # of first sample. 0 => 1 NCOUNT 0.0 30000.0 # of sample. 0 => 1 page. WTUV 0.0 1000.0 Scale UVW by * WTUV 0 => 1000 OPTYPE Choice of format type: 'HOLG' write holography file else print holography data NPOINTS 0.0 1000.0 Number of samples to keep at the end of each pointing Used if APARM = 0 0 => 100 APARM (1) 0 => NPOINTS used 1 => APARM(2,3) used (2) number of samples dropped at the beginning of each pointing (3) number of samples dropped at the end of each pointing BDROP 0.0 1000.0 Minimum number of samples to keep the pointing at all DOCRT -1.0 132.0 > 0 -> use the terminal, else use the line printer > 72 => terminal width OUTPRINT Printer disk file to save BADDISK Disk to avoid for scratch. ---------------------------------------------------------------- UVHOL Type: Task Use: Prints holography data from a u,v data base, optionally making retained text files. UVHOL is similar to UVPRT, but does only the special holography modes which used to be a part of UVPRT. These include printing for display purposes and the ability to write files for input to HOLGR. Adverbs: USERID.....Input file user number. 0 => logon user, 32000 => any user. INNAME.....Input UV file name (name) Standard defaults. INCLASS....Input UV file name (class) Standard defaults. INSEQ......Input UV file name (seq. #) 0 => highest. INDISK.....Disk drive # of input UV file. 0 => any. SOURCES....List of sources to be printed. ' '=> all; if any starts with a '-' then all except ANY source named. QUAL.......Qualifier of source to be printed. -1 => all. CALCODE....Calibrator code of sources to print. ' '=> all. STOKES.....The usual Stokes parameter. In HOLG mode, FULL means to write all 4 polarizations to disk files, IQUV means to write all 4 Stokes polarizations, IV means to write the two parallel hand Stokes, otherwise RR and LL only are written. When simply printing, STOKES beginning with I means 'IQUV', otherwise FUULL is used. SELBAND....Bandwidth of data to be selected. If more than one IF is present SELBAND is the width of the first IF required. Units = kHz. For data which contain multiple bandwidths/frequencies the task will insist that some form of selection be made by frequency or bandwidth. SELFREQ....Frequency of data to be selected. If more than one IF is present SELFREQ is the frequency of the first IF required. Units = MHz. FREQID.....Frequency identifier to select (you may determine which is applicable from the OPTYPE='SCAN' listing produced by LISTR). If either SELBAND or SELFREQ are set, their values overide that of FREQID. However, setting SELBAND and SELFREQ may result in an ambiguity. In that case, the task will request that you use FREQID. If all SELBAND, SELFREQ and FREQID are not specified (.le. 0) then all FQ ids will be selected. TIMERANG...Time range of the data to be printed. In order: Start day, hour, min. sec, end day, hour, min. sec. Days relative to reference date. ANTENNAS...A list of the antennas to print. If any number is negative then all antennas listed are NOT desired and all others are. All 0 => list all. For HOLO and HOLG modes, ANTENNAS is a list of reference antennas. The first is used to name the output file in HOLG mode. BASELINE...Baselines are specified using BASELINE. E.g. for baselines 1-6,1-8, 2-6 and 2-8, use ANTENNAS=1,2; BASELINE=6,8. For HOLO and HOLG modes, BASELINE(1-50) are the moving antennas (no default for BASELINE(1)). The task will loop doing one ANTENNAS(n)-BASELINE(1) pair at a time until a 0 is found in the list of ANTENNASs. Then it loops with all ANTENNAS(n) to BASELINE(2) etc. until a zero is found in BASELINE. UVRANGE....Range of projected spacings to be printed in 1000's of wavelengths. 0 => 1, 1.E10 SUBARRAY...Subarray number to print. 0 => 1. CHANNEL....Spectral line channel number. 0 => 1. BIF........IF number to print. 0 => 1 DOCALIB....If true (>0), calibrate the data using information in the specified Cal (CL) table for multi-source or SN table for single-source data. If > 1.5, also calibrate the weights (new for VLA, normal for VLBI). GAINUSE....Version number of the Cal. table to apply to the data if DOCALIB=1. Refers to a CL table for multi-source data or an SN table for single source. 0 => highest. DOPOL......If > 0 then correct data for instrumental polarization as represented in the AN table. Only one subarray may be done at a time. This correction is only useful if PCAL has been run or feed polarization parameters have been otherwise obtained. See HELP DOPOL for available correction modes. BLVER......Version number of the baseline based calibration (BL) table to apply. <0 => apply no BL table, 0 => highest. FLAGVER....Specifies the version of the flagging table to be applied. 0 => highest numbered table. <0 => no flagging to be applied. DOBAND.....(multisource) If true (>0) then correct the data for the shape of the antenna bandpasses using the BP table specified by BPVER. The correction has five modes: (a) if DOBAND=1 all entries for an antenna in the table are averaged together before correcting the data. (b) if DOBAND=2 the entry nearest in time (including solution weights) is used to correct the data. (c) if DOBAND=3 the table entries are interpolated in time (using solution weights) and the data are then corrected. (d) if DOBAND=4 the entry nearest in time (ignoring solution weights) is used to correct the data. (e) if DOBAND=5 the table entries are interpolated in time (ignoring solution weights) and the data are then corrected. BPVER......(multi-source) specifies the version of the BP table to be applied. 0 => highest numbered table. SMOOTH.....Specifies the type of spectral smoothing to be applied to a uv database . The default is not to apply any smoothing. The elements of SMOOTH are as follows: SMOOTH(1) = type of smoothing to apply: 0 => no smoothing 1 => Hanning 2 => Gaussian 3 => Boxcar 4 => Sinc (i.e. sin(x)/x) SMOOTH(2) = the "diameter" of the function, i.e. width between first nulls of Hanning triangle and sinc function, FWHM of Gaussian, width of Boxcar. Defaults (if < 0.1) are 4, 2, 2 and 3 channels for SMOOTH(1) = 1 - 4. SMOOTH(3) = the diameter over which the convolving function has value - in channels. Defaults: 1, 3, 1, 4 times SMOOTH(2) used when input SMOOTH(3) < net SMOOTH(2). BCOUNT.....Start listing at the BCOUNT'th data point selected BEFORE applying the above criteria. (N.b. this is a change made 2 May 1997; previously BCOUNT applied after application of the other selection criteria.) Ignored (set to 1) for HOLG. NCOUNT.....List NCOUNT data points (after all data selection has been applied). 0 => 1 page listed. UVHOL will list up to 30000 visibilities. This limit does not apply to HOLG and applies on a per antenna-pair basis for HOLO. Be aware that UVHOL now goes through the data to be printed twice, once to determine the u-v-w, data, and weight ranges and the second time to print things. Using NCOUNT to reduce the time required by the first pass helps when DOCRT is true. WTUV.......Scale the U, V, and W values in wavelengths by multiplying by WTUV. 0 => 0.001, i.e. Kilo wavelengths for non-HOLO modes. For HOLO, 0 => 1000. for U and V and 1.0 for W. Set to 1 for HOLG. OPTYPE.....OPeration code to change details of the format: 'HOLG' => write holography data from one or more antenna pairs to 2 or 4 files per pair for use in HOLGR. (No normal printing is done.) otherwise => print only holography data from one or more antenna pairs. NPOINTS....Retain the last NPOINTS samples from each pointing. Note that pointings are indicated by the W term in the U,V,W triplet. For holography, W = 40000+X where X is a counter referring to the pointing or dwell currently selected. The first samples for each dwell are suspect since not all antennas have settled down. This option allows you to select only the last NPOINTS samples. 0 -> 100 (the upper limit). APARM......(1) 0 => option determined by NPOINTS is used 1 => option determined by APARM(2,3) is used (2) number of samples dropped at the beginning of each pointing (3) number of samples dropped at the end of each pointing BDROP......If a pointing appears to fewer than BDROP samples, then drop it entirely. < 1 -> 5 DOCRT......False (<= 0) use the line printer if OUTPRINT = ' ' else write named OUTPRINT file only. True (> 0) use the terminal interactively. The task will use the actual terminal width as a display limit unless 72 < DOCRT < width. In that case, the display limit will be DOCRT characters. 132 width is best. OUTPRINT...Disk file name in which to save the line printer output. ' ' => use scratch and print immediately for interactive jobs - batch jobs use OUTPRINT = 'PRTFIL:BATCHjjj.nnn' (jjj= job #, nnn = user #). When OUTPRINT is not blank, multiple outputs are concatenated, and the file is not actually printed. For HOLG mode only, OUTPRINT must be non-blank and must give the name of a logical area to which to write the HOLGR data files (e.g. OUTPR = 'MYAREA' or OUTPR = 'MYAREA:xxx', where xxx can be anything and MYAREA is a logical area defined before starting AIPS in the usual way). If OUTPRINT gives only a logical name, then the name HOLOnn-mmppii is used where nn is the reference antenna (BASELINE(j)), mm is the antenna (or 0 if multiple), pp are 2 letters giving the polarization, and ii id the IF. If xxx is not blank, then the output name is xxx (any number of letters) with ppii concatenated. BADDISK....Disk numbers to avoid for scratch files. Scratch files may be created by the sorting routines if calibration or flagging is applied. ---------------------------------------------------------------- Special notes on holography data, in HOLO or HOLG modes: (1) Any included data that does not have a W > 40000 is assumed to be calibrator data and is ignored. (2) The W term is expected to be 40000 + 256*qualifier + mode, where mode is supposed to be > 0. When mode is 0, the data are assumed to be taken during an antenna turn-around phase and are discarded. The first mode 1 directly after a mode 0 is also discarded. (3) When printing in these modes, the 40000 and n*256 parts of W are dropped. ----------------------------------------------------------------