*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.*
Fills the model column for flux density calibrators:
The task places the model visibility amp and phase associated
with a specified clean components image into the model column
of the data set. The simplest way is to enter the flux density
(I,Q,U,V) explicitly.
Models are available for 3C48, 3C138, and 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 models are
presently available.
The location of the models are system dependent: At the AOC, the
models are in the directory::/usr/lib/casapy/data/nrao/VLA/CalModels
ssoflux need only be run on the calibrator sources with a know 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).
[run listobs to obtain the list id's or names of calibrators]
default: ''=all fields
Only one field can be used if a source model or specific fluxdensity
is inserted.
If field string is a non-negative integer, it is assumed a field index
otherwise, it is assumed 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'; fields 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
modimage -- Optional model image (I only) from which the model visibilities
are calculated and placed in the model column. Each field must
be done separately. The image flux density will be scaled from the
frequency in the model to that actually used.
In CV and the AOC, the models are located in the
/usr/lib/casapy/data/nrao/VLA/CalModels directory
fluxdensity -- Specified flux density [I,Q,U,V] in Jy
default => -1, puts total flux density for known standard source
places [1,0,0,0] for any other source.
Otherwise, places the specified flux density for the source. This
is the only way to insert a polarized flux density model at the
present time (March 2008).
example: fluxdensity=[2.63,0.21,-0.33,0.02]
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'
1.8.0