AIPS HELP file for BSMOD in 31DEC22
As of Wed Jan 19 12:06:30 2022
BSMOD: Task to create model beam-switched data sets
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 #.
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)
CPARM 1. Time increment (sec) 1/4
2, Fly-back time 60
3. Start hour angle (hrs)
4. RA (deg)
5. Dec (deg)
6. Telescope diameter
7. Observatory longitude
8. Observatory latitude
9. Observatory distance
APARM X: npix, sep, noise
Y: npix, sep, noise
FLUX -1.0 100.0 RMS noise (K) added to model
BPARM 1: Official beam throw
2: Throw scale factor 0 -> 1
3: Rotate throw CCW (degrees)
4: Record true position
5: Ratio +/- beam gain 0->1
6: Ratio +/- beam width 0->1
REFDAT 'yyyymmdd' of observation
OBJECT Source name
Task: This task creates a pair of beam-switched data sets from a model
plus sky noise. The model consists of up to four Gaussians, each
of which will be convolved with the single-dish beam width given
by an adverb. Instrumental defects including pointing error,
beam throw length and angle error, and beam relative gain and
width error may be simulated.
The NRAO 12m telescope is used as the example dish.
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.
NGAUSS.....Number of sources in model: 1 - 4
GMAX.......Peak brightness of component in the units of the "uv" data
(normally Kelvins). The peak used is GMAX if the component or
the antenna beam have 0 width, otherwise it is reduced by
the ratio of the area of the input component to the
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
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.
CPARM......(1) Time increment (sec) 0 -> 1/4
(2) Fly-back time (sec) 0 -> 60
(3) Start hour angle (hrs)
(4) RA (deg)
(5) Dec (deg)
(6) Telescope diamter (m)
(7) Observatory (telescope) longitude (degrees)
(8) Observatory (telescope) latitude (degrees)
(9) Observatory distance to center of earth (m)
If 7, 8, or 9 are 0, then the NRAO 12m (-111.6, 31.78,
6374166) are assumed.
APARM......(1) Horizontal coordinate: Number samples
(2) Horizontal coordinate: sample separation (arcsec)
telescope moves 1 plus beam / sample
(3) Horizontal coordinate: coord noise (arcsec)
(4) Vertical coordinate: Number samples
(5) Vertical coordinate: sample separation (arcsec)
(6) Vertical coordinate: coord noise (arcsec)
(7) Beam size (arcsec)
FLUX.......Add to the model noise of rms = FLUX in the units of the uv
data (usually K)
BPARM......Parameters for modeling beam-switched continuum data.
(1) Beam throw (arcsec)
(2) Correction factor for the throw. 0 => 1
(3) Rotation of throw from horizontal CCW in degrees.
(4) > 0 => record actual coordinates not commanded ones.
(5) Ratio of plus beam to minus beam gains. 0 -> 1.
(6) Ratio of plus beam to minus beam widths. 0 -> 1.
REFDATE....'yyyymmdd' of observation. ' ' => '20000101'
OBJECT.....Source name to use.