; DOVLAMP ;--------------------------------------------------------------- ;! Produces amp calibration file for phased-VLA VLBI data ;# RUN POPS VLBI VLA UTILITY CALIBRATION ;----------------------------------------------------------------------- ;; Copyright (C) 2015-2016 ;; 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 ;----------------------------------------------------------------------- ;--------------------------------------------------------------- DOVLAMP LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC DOVLAMP : Procedure to produce ANTAB-style file for phased-VLA ASDMFILE Full path name to ASDM dir. CONFIG 0.0 Select this "configuration" INNAME In/output file name INCLASS In/output file class INSEQ In/output file sequence num INDISK Disk # for in/output file BIF 0.0 100.0 Lowest IF number 0=>all EIF 0.0 100.0 Highest IF number 0=>all CALSOUR FOR FLUX CALIBRATOR ONLY REFANT Reference antenna OUTTEXT Directory to put output file ---------------------------------------------------------------- DOVLAMP Type: Procedure Use: This procedure us usually used by NRAO operations to make phased-VLA VLBI amplitude calibration files and is not intended for general usage. However people with phased-VLA data might want to improve on their amplitude calibration by, for example, flagging the switched power before running this procedure. This procedure optionally loads a SDM (VLA) file and then makes amplitude calibration information for the phased Jansky VLA (observed after February 2011) when it is used as a VLBI element. The procedure processes the VLA only data from WIDAR and using the switched power and optional primary amplitude calibrator to produce a text file that can be loaded into the TY and GC table of the VLBI data with ANTAB. Type RUN DOVLAMP to define the DOVLAMP procedure. ASDMFILE...To load the data automatically from disk, set this. The full path name to and including the top directory of the ASDM/BDF data. Two 64-character strings may be used for long names. The ASDMFILE(2) will be appended to the non-blank portion of ASDMFILE(1) to generate the name used. The code will also manage when ASDMFILE(1) begins with either '$xxxx/' or 'xxxx:' where xxxx is a logical (environment) variable. The filename sent to OBIT will be the translation of $xxxx followed by a '/' followed by an remaining non-blank characters in ASDMFILE(1) followed by ASDMFILE(2). If ASDMFILE is set then CONFIG, INNAME, INCLASS and INSEQ must be set. If ASDMFILE is set and INCLASS='TYAPL' it is assumed that the data is loaded and ASDMFILE will be ignored. CONFIG.....ASDM files often contain more than one "configuration" numbered from 0 to N. Configurations may differ in observing band, number of spectral windows, number of spectral channels in the spectral windows, etc. Use BDFLIST to see what configurations are in your data set. DOVLAMP can load only one configuration at a time. INNAME.....The name of the file to be processed. If ASDMFILE is set then this will be the output name. INCLASS....The class of the file to be processed. If ASDMFILE is set then this will be the output class. If INCLASS='TYAPL' then it is assumed that the data has already been loaded and TYAPL has been run so the data will not be loaded even if ASDMFILE is set, and TYAPL will not run it again. INSEQ......The sequence number of the file to be processed. Zero defaults to the highest sequence number of a file matching INNAME, INCLASS, and INDISK. If ASDMFILE is set then this will be the output sequence. INDISK.....The disk drive number of the file to be corrected. BIF........First IF to copy with UVCOP then process. 0=>all. EIF........Highest IF to copy. 0=>all higher than BIF CALSOUR....Primary flux calibrator, if present in observations, if left blank a primary flux calibrator will be searched for in the SU table. If CALSOUR(1)='NOCAL', then a calibrator will not be searched for. REFANT.....Reference antenna. OUTTEXT....Directory to put output file. Path or environmental variable will work. The name of the output file is automatically generated. The path must be shorter than 27 characters (including final /). ---------------------------------------------------------------- DOVLAMP: Procedure to create a-priori calibration for the phased VLA Documentor: Amy Mioduszewski Related Programs: VLAMP, CALIB, CLCAL, CALRD, TYAPL This procedure is intended to produce the amplitude calibration for the phased VLA (after February 2011) when it is used as a VLBI element. The VLA data can be loaded from disk, if needed. It produces a text file that can be loaded with ANTAB. The main task used in DOVLAMP is VLAMP, which takes the switched power converts that to the system temperature (Tsys) and then takes the harmonic sum of the Tsys over all the antennas multiplied by the amplitude in the first CL table. The amplitude in the first CL table has the gain curve polynomial in it. The "Gain" (which really isn't the gain because some of that is folded into the harmonic sum of the Tsys) is the sum of the sensitivities of the antennas in the GC table. Then VLAMP makes the ANTAB style text file that can be loaded into the VLBI data. DOVLAMP adds some steps in order to improve the calibration. If a primary amplitude calibrator was observed (3C286, 3C48, 3C147, 3C138 or 3C295) then it will be used to improve the calibration. This calibrator can either be specified in CALSOUR or, if CALSOUR is blank, will be found automatically in the SU table. If INCLASS='TYAPL' then it is assumed that TYAPL has been run and the procedure will not run it again. This is useful if there has been an problem later in the procedure since the run of TYAPL is usually the longest part of the procedure. Basic steps of procedure: 0) Perform basic checks on inputs 1) Determine if file needs to be loaded (i.e., is ASDMFILE set) --Yes, run BFD2AIPS, user INNAME, INCLASS and INSEQ as output name --No, run rest of script on file set in INNAME, INCLASS and INSEQ 2) If BIF and/or EIF are not equal to 0 then --run UVCOP to copy BIF-EIF and proceed with UVCOPed file 3) If INCLASS is *not* TYAPL then --run TYSMO to clip bad points in SY table --run TYAPL From now on everything is done to the TYAPL file: 4) If CALSOUR is not set, search for standard VLA flux calibrator (3C48, 3C138, 3C147, 3C286 or 3C295) in the SU table. 5) If flux calibrator exists in data then: --Load model for flux calibrator is one exists in the data --run SETJY on flux calibrator --run CALIB on flux calibrator --zero phases on CALIB solutions (want amp only) --run CLCAL to apply amp corrections to first CL table 6) Run VLAMP to create ANTAB style file.