https://casaguides.nrao.edu/index.php?title=Setjy&feed=atom&action=historySetjy - Revision history2024-03-29T11:49:10ZRevision history for this page on the wikiMediaWiki 1.38.6https://casaguides.nrao.edu/index.php?title=Setjy&diff=16920&oldid=prevJott: Replaced content with "{{setjy}}"2015-05-18T20:38:16Z<p>Replaced content with "{{setjy}}"</p>
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</td></tr></table>Conversion scripthttps://casaguides.nrao.edu/index.php?title=Setjy&diff=1142&oldid=prevLchomiuk at 18:23, 11 February 20102010-02-11T18:23:14Z<p></p>
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</table>Lchomiukhttps://casaguides.nrao.edu/index.php?title=Setjy&diff=70&oldid=prevJgallimo: Created page with '<pre> Fills the model column with the visibility of a calibrator The task places the model visibility amp and phase associated with a specified source (generally a…'2009-10-30T14:54:21Z<p>Created page with '<pre> Fills the model column with the visibility of a calibrator The task places the model visibility amp and phase associated with a specified source (generally a…'</p>
<p><b>New page</b></p><div><pre><br />
Fills the model column with the visibility of a calibrator<br />
<br />
The task places the model visibility amp and phase associated<br />
with a specified source (generally a calibrator).<br />
The simplest way to to enter the flux density<br />
(I,Q,U,V) explicitly, but this is valid only for a point source.<br />
<br />
For an extended source, the clean model (image.model) can be<br />
specified and the model visibilities associated with this clean<br />
model is placed in the visibility model column.<br />
<br />
Models are available for 3C48, 3C138, 3C286 between<br />
1.4 and 43 GHz. 3C147 is available above 13 GHz. These models<br />
are scaled to the precise frequency of the data. Only I source <br />
model can be inserted at a time.<br />
<br />
The location of the models are system dependent: At the AOC and CV,<br />
the models are in the directory::/usr/lib/casapy/data/nrao/VLA/CalModels<br />
or /usr/lib64/casapy/data/nrao/VLA/CalModel.<br />
<br />
Setjy need only be run on the calibrator sources with a know flux<br />
density and/or model.<br />
<br />
Keyword arguments:<br />
vis -- Name of input visibility file<br />
default: none. example: vis='ngc5921.ms'<br />
field -- Select field using field id(s) or field name(s).<br />
default: ''=all fields, but run setjy one field at a time.<br />
[run listobs to obtain the list id's or names of calibrators]<br />
If field string is a non-negative integer, it is assumed a field index<br />
otherwise, it is assumed a field name<br />
field='0~2'; field ids 0,1,2<br />
field='0,4,5~7'; field ids 0,4,5,6,7<br />
field='3C286,3C295'; field named 3C286 adn 3C295<br />
field = '3,4C*'; field id 3, all names starting with 4C<br />
spw -- Select spectral window/channels<br />
default: ''=all spectral windows and channels<br />
spw='0~2,4'; spectral windows 0,1,2,4 (all channels)<br />
spw='<2'; spectral windows less than 2 (i.e. 0,1)<br />
spw='0:5~61'; spw 0, channels 5 to 61<br />
spw='0,10,3:3~45'; spw 0,10 all channels, spw 3, channels 3 to 45.<br />
spw='0~2:2~6'; spw 0,1,2 with channels 2 through 6 in each.<br />
spw='0:0~10;15~60'; spectral window 0 with channels 0-10,15-60<br />
spw='0:0~10,1:20~30,2:1;2;4'; spw 0, channels 0-10,<br />
spw 1, channels 20-30, and spw 2, channels, 1,2 and 4<br />
field='3C286,3C295'; field named 3C286 adn 3C295<br />
field = '3,4C*'; field id 3, all names starting with 4C<br />
spw -- Select spectral window/channels<br />
default: ''=all spectral windows and channels<br />
spw='0~2,4'; spectral windows 0,1,2,4 (all channels)<br />
spw='<2'; spectral windows less than 2 (i.e. 0,1)<br />
spw='0:5~61'; spw 0, channels 5 to 61<br />
spw='0,10,3:3~45'; spw 0,10 all channels, spw 3, channels 3 to 45.<br />
spw='0~2:2~6'; spw 0,1,2 with channels 2 through 6 in each.<br />
spw='0:0~10;15~60'; spectral window 0 with channels 0-10,15-60<br />
spw='0:0~10,1:20~30,2:1;2;4'; spw 0, channels 0-10,<br />
spw 1, channels 20-30, and spw 2, channels, 1,2 and 4<br />
<br />
Use one of the two methods below: modimage or fluxdensity<br />
<br />
modimage -- Model image (I only) from which the model visibilities<br />
default: '' means do not use model, but fluxdensity<br />
Each field must be done separately. The image clean model<br />
will be scaled from the frequency in the model to that actually used.<br />
Both the amplitude and phase are calculated.<br />
At the AOC or CV, the models are located in the<br />
/usr/lib/casapy/data/nrao/VLA/CalModels/3C286_L.im (egs)<br />
lib64<br />
<br />
fluxdensity -- Specified flux density [I,Q,U,V] in Jy<br />
default => -1, places [1,0,0,0] flux density for all sources,<br />
except for 3C286, 3C48 and 3C147 where the absolute flux<br />
density it added. It is recommended to use the modimage for<br />
these sources if they are resolved with the observations.<br />
Only one flux density can be executed at a time. The phases are<br />
set to zero.<br />
example fluxdensity=-1 will insert 1.0 for all calibrators<br />
except 3C286, 3C147 and 3C48<br />
example field = '1'; fluxdensity=[3.2,0,0,0] wil put in <br />
flux density of I=3.2 for field='1'<br />
<br />
At present, this is the only method to insert a polarized flux<br />
density model (June 2000).<br />
example: fluxdensity=[2.63,0.21,-0.33,0.02]<br />
will put in I,Q,U,V flux densities of 2.63,0.21,-0.33,<br />
and 0.02, respectively, in the model column.<br />
<br />
standard -- Flux density standard, used if fluxdensity<0<br />
default: 'Perley-Taylor 99'; example: standard='Baars'<br />
Options: 'Baars','Perley 90','Perley-Taylor 95',<br />
'Perley-Taylor 99'<br />
</pre></div>Jgallimo