; SDMOD ;--------------------------------------------------------------- ;! modifies single-dish UV data with model sources ;# TASK UV SINGLEDISH MODELING ;----------------------------------------------------------------------- ;; Copyright (C) 1995-1996, 2000 ;; 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 ;----------------------------------------------------------------------- SDMOD LLLLLLLLLLLLUUUUUUUUUUUU CCCCCCCCCCCCCCCCCCCCCCCCCCCCC sdmod Task to add model sources to single-dish data INNAME Input UV file name INCLASS Input UV file class INSEQ 0.0 9999.0 Input UV file seq. # INDISK 0.0 9.0 Input UV file disk unit # IN2NAME Input model image name IN2CLASS Input model image class IN2SEQ 0.0 9999.0 Input model image seq. # IN2DISK 0.0 9.0 Input model image disk # OUTNAME Output UV file name OUTCLASS Output UV file class OUTSEQ -1.0 9999.0 Output UV file seq. # OUTDISK 0.0 9.0 Output UV file disk unit #. OPTYPE 'IMAG' => use model image else use Gaussians BCHAN 0.0 9999. First channel to include ECHAN 0.0 9999. Last channel to include BIF 0.0 999. First IF to include EIF 0.0 999. Last IF to include NGAUSS 0.0 4.0 Number of components GMAX Peak of component (K) GPOS (X,Y) position (arc sec) GWIDTH (BMAJ, BMIN, BPA) of comp. (arc sec, arc sec, deg) APARM Center channel, fwhm for each component. 0 => chan indep. FLUX -1.0 100.0 >= 0 RMS noise (K) to add to model; < 0 add model to data BPARM 1: >0 => beam-switched cont. 2: Throw scale factor 0 -> 1 3: Rotate throw CCW (degrees) 4: RA or Az increment 5: Dec or El increment 6: RA or Az shift 7 Dec or El shift 8: > 0 Coordinates corrected before model computation ---------------------------------------------------------------- SDMOD Task: This task will SUBTRACT a model FROM single-dish "uv" data (if FLUX < 0) or replace those data with a model plus random noise. The model consists of up to four Gaussians, each of which will be convolved with the "Clean beam" parameters in the data header which are meant in this case to be the single-dish beamwidth. Alternatively, the model can be an image which is subtracted from the data or which replaces the data. Adverbs: 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. IN2NAME....Input model image name (name). Standard defaults. IN2CLASS...Input model image name (class). Standard defaults. IN2SEQ.....Input model image name (seq. #). 0 => highest. IN2DISK....Disk drive # of input model image. 0 => any. OUTNAME....Output UV file name (name). Standard defaults. 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 with space for the file. OPTYPE.....Operation: 'IMAG' => use IN2NAME et al. to provide an image of the model (taken to be a continuum image) BCHAN......First spectral channel to include: 0 => 1 ECHAN......Last spectral channel to include: 0 => highest BIF........First IF to include: 0 => 1 EIF........Last IF to include: 0 => highest. NGAUSS.....Number of sources in model: 1 - 4 Used if OPTYPE is not 'IMAG' . GMAX.......Peak brightness of component in the units of the "uv" data (normally Kelvins). To subtract a component from the data, set GMAX < 0. The peak used is GMAX if the component or the antenna beam have 0 width, otherwise it is reduced by the ration of the area of the input component to the convolved component. GPOS.......(X,Y) position of the component in arc seconds from the reference position. GPOS(1,*)/cos(declination) is the offset in right ascension, (> 0 -> the component is East of the reference point) and GPOS(2,*) is the offset in declination (> 0 place the component North of the refernce position.) GWIDTH.....The Gaussian widths: GWID(1,*) is the major axis, GWID(2,*) is the minor axis both in arc sec and GPOS(3,*) is the position angle (from North to East to major axis) in degrees. Each component will be convolved with the single-dish beam width (found in the header) before being applied to the data. APARM......List of center and fwhm in channels (in the input uv data set) for Gaussian spectral form for the components. A width of zero => channel independent. Thus 29, 3, 37, 5, 0 specifies the first 2 components are also Gaussian in channels centered on input channels 29 and 37 with fwhms of 3 and 5 channels, and the other 2 components (if any) are constant in frequency. FLUX.......>= 0 => Replace the input data with the model plux noise of rms = FLUX in the units of the uv data (usually K) < 0 => Add the model (with no noise) to the input data. FLUX is used with both Gaussians and IMAGe. BPARM......Parameters for modeling beam-switched continuum data. (1) > 0 => these are such data. The main effect of this is to include the throw and to ignore the recorded center coordinate. The channel adverbs are ignored. (2) Correction factor for the throw. 0 => 1 (3) Rotation of throw from horizontal CCW in degrees. Parameters applying to all data sets: (4) RA or Az increment in arc seconds (0 => none). The coordinates are forced to be the nearest integer multiples of this increment. (5) Dec or El increment in arc seconds (0 => none). The coordinates are forced to be the nearest integer multiples of this increment. (6) RA or Az shift in arc seconds applied after the increment correction. (7) Dec or El shift in arc seconds applied after the increment correction. (8) > 0 => correct the coordinates and then compute the model, else compute the model and then correct the coordinates. ----------------------------------------------------------------