Fills the model column with the visibilities of a calibrator
*This is an experimental clone of setjy while flux calibration with
Solar System objects is being tested. It will eventually be merged
back into setjy.*
This task sets the model visibility amp and phase of a
specified source (generally a calibrator). The simplest way is
to enter the flux density (I,Q,U,V) explicitly, but this is
valid only for a point source.
For an extended source, the clean model (image.model) can be
specified and the model visibilities associated with this clean
model is placed in the visibility model column.
Models are available for 3C48, 3C138, 3C286 between
1.4 and 43 GHz. 3C147 is available above 13 GHz. These models
are scaled to the precise frequency of the data. Only I source
model can be inserted at a time.
The location of the models are system dependent: At the AOC and CV,
the models are in the directory::/usr/lib/casapy/data/nrao/VLA/CalModels
or /usr/lib64/casapy/data/nrao/VLA/CalModel.
ssoflux need only be run on the calibrator sources with a known flux
density and/or model.
Keyword arguments:
vis -- Name of input visibility file
default: none. example: vis='ngc5921.ms'
field -- Select field using field id(s) or field name(s).
default: ''=all fields, but run ssoflux one field at a time.
[run listobs to obtain the list id's or names of calibrators]
If field is a non-negative integer, it is assumed to be a field
index. Otherwise, it is taken to be a field name.
field='0~2'; field ids 0,1,2
field='0,4,5~7'; field ids 0,4,5,6,7
field='3C286,3C295'; field named 3C286 and 3C295
field = '3,4C*'; field id 3, all names starting with 4C
spw -- Select spectral window/channels
default: ''=all spectral windows and channels
spw='0~2,4'; spectral windows 0,1,2,4 (all channels)
spw='<2'; spectral windows less than 2 (i.e. 0,1)
spw='0:5~61'; spw 0, channels 5 to 61
spw='0,10,3:3~45'; spw 0,10 all channels, spw 3, channels 3 to 45.
spw='0~2:2~6'; spw 0,1,2 with channels 2 through 6 in each.
spw='0:0~10;15~60'; spectral window 0 with channels 0-10,15-60
spw='0:0~10,1:20~30,2:1;2;4'; spw 0, channels 0-10,
spw 1, channels 20-30, and spw 2, channels, 1,2 and 4
Use one of the two methods below: modimage or fluxdensity
modimage -- Model image (I only) for setting the model visibilities.
default: '' means use fluxdensity instead of modimage.
Each field must be done separately. The image clean model
will be scaled from the frequency in the model to that actually used,
unless fluxdensity = 0 (or fluxdensity[0] = 0).
Both the amplitude and phase are calculated.
At the AOC or CV, the models are located in
/usr/lib/casapy/data/nrao/VLA/CalModels/3C286_L.im (egs)
lib64
fluxdensity -- Specified flux density [I,Q,U,V] in Jy
default: -1, uses [1,0,0,0] flux density for all sources,
except for 3C286, 3C48 and 3C147, which use standard flux
densities. It is recommended to use modimage for
these sources if they are resolved by the observation.
Only one flux density can be specified at a time. The phases are
set to zero.
example fluxdensity=-1 will insert 1.0 for all calibrators
except 3C286, 3C147 and 3C48.
example field = '1'; fluxdensity=[3.2,0,0,0] wil put in
a flux density of I=3.2 for field='1'
At present (June 2000), this is the only method to insert a
polarized flux density model.
example: fluxdensity=[2.63,0.21,-0.33,0.02]
will put in I,Q,U,V flux densities of 2.63,0.21,-0.33,
and 0.02, respectively, in the model column.
standard -- Flux density standard, used if fluxdensity<0
default: 'Perley-Taylor 99'; example: standard='Baars'
Options: 'Baars','Perley 90','Perley-Taylor 95',
'Perley-Taylor 99', 'Perley-Butler 2010',
and 'Butler-JPL-Horizons 2010'.
All but the last one are for extragalactic calibrators,
and the final one is for Solar System objects.
1.8.0