; SDTUV ;--------------------------------------------------------------- ;! Task to convert SD table files to UV like data. ;# TASK SINGLEDISH ;----------------------------------------------------------------------- ;; Copyright (C) 1995 ;; 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 ;----------------------------------------------------------------------- ;--------------------------------------------------------------- SDTUV LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC SDTUV Task to convert SD table files to UV like data. INNAME Input SD table file name. INCLASS Input SD table file class INSEQ -1.0 9999.0 Input SD table file seq. # INDISK 0.0 9.0 Input SD table file disk #. INEXT Input table extension type INVERS Input table file version no. OUTNAME Output UV file name (name) OUTCLASS Output UV file name (class) OUTSEQ -1.0 9999.0 Output UV file name (seq. #) OUTDISK 0.0 9.0 Output UV file disk unit #. APARM Control info: 1 = CS table interval 0=none 2 .ge. 0 => SCAN rand. parm. 3 .gt. 0 => spline fitting 4 Spline smoothness parm. 5 .gt. 0 => median win. width 7 Max. dev. per receiver 8 Max. no. rcx. exceeding (7) BPARM Task enrichment parm. 1 .gt. 0 => replace bad RA's 2 .gt. 0 => beam for lat. foc 3 .gt. 0 => patch 140 ft dec. ARRAY2 Baseline table (20,2) (i,1) = declination i (i,2) = baseline i ---------------------------------------------------------------- SDTUV Task: This task will create an AIPS uv data file and fill it by converting a single dish table to uvlike data. If requested, CS (calibration) and NX (index) tables will be created and filled. Several filtering methods are available for removing a baseline from the data. Adverbs: INNAME.....Input SD table file name (name). INCLASS....Input SD table file name (class). INSEQ......Input SD table file name (seq. #). INDISK.....Disk drive # of input table file. INEXT......Table extension type. ' '=>'SD' INVER......Table extension version. 0=> convert all. OUTNAME....Output UV file name (name). Standard behavior with default 'UV DATA FILE'. OUTCLASS...Output UV file name (class). Standard defaults. OUTSEQ.....Output UV file name (seq. #). 0 => highest unique. OUTDISK....Disk drive # of output UV file. 0 => highest disk with space for the file. APARM......Control info: 1 = CS table interval in min. If < 0 then no CS or NX tables are written. 2 If the value is .ge. 0 then SCAN and SAMPLE random parameters are added if appropriate. 3 If the value is greater than 0 then a cubic spline is fitted to the median value in blocks APARM(3) samples long. The spline is then used to subtract the baseline. 4 Smoothness factor, any positive number. Larger values give better fit, smaller a smoother curve. 0 => 1. 5 If the value is larger than 0 then the median value in a sliding window APARM(5) samples wide is used as an estimate of the baseline and removed. 7,8 If the value of (7) is larger than 0 then an interference detector is invoked. For each time sample and receiver the difference between the value and the mean of the preceeding and following time samples is computed. If more than APARM(8) receivers have a difference exceeding APARM(7) then that time sample is flagged. BPARM......If BPARM(1) .gt. 0 then the 300 foot bad RA problem will be patched up. If BPARM(2) .gt. 0 then a gain correction will be made for the lateral (off axis) defocusing error. BPARM(2) is the beam offset (degrees) that gives 3 dB loss in gain (field of view). If BPARM(3) .gt. 0 then the declination error in the 140 ft telescope pointing program will be patched. ARRAY2.....This contains a table of baselines to subtract as a function of declination. This is mostly useful for Meridian transit measurments. Baseline temperatures to be removed can be specified at up to 20 arbitrary declinations. The range of declinations in the table MUST enclose all declinations present in the data and at least 3 points must be included. The order is in ascending (north positive) declination. A cubic spline interpolation is used. ARRAY2(i,1) = declination i ARRAY2(i,2) = baseline temperature i. ----------------------------------------------------------------