Jupiter: continuum polarization calibration 6.4.1: Difference between revisions
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<b>NOTE</b>: If you are using CASA 4.7 or earlier, you may want to use <tt>poltype='X'</tt> in X-term calculations (Mueller matrices). For CASA 5.0 and later this option will not work (the relevant CASA documentation is being updated), and hence you need to use <tt>poltype='Xf'</tt> (Jones matrices). Although 'Xf' should be used predominantly for large bandwidths, which clearly is not the case here, it can also be used for the single channel old VLA data as long as you make sure the <tt>interp</tt> parameter is set to default (which should be <tt>nearest</tt>). | <b>NOTE</b>: If you are using CASA 4.7 or earlier, you may want to use <tt>poltype='X'</tt> in X-term calculations (Mueller matrices). For CASA 5.0 and later this option will not work (the relevant CASA documentation is being updated), and hence you need to use <tt>poltype='Xf'</tt> (Jones matrices). Although 'Xf' should be used predominantly for large bandwidths, which clearly is not the case here, it can also be used for the single channel old VLA data as long as you make sure the <tt>interp</tt> parameter is set to default (which should be <tt>nearest</tt>). | ||
=== Apply the | === Apply the Calibration === | ||
Now that we have derived all the calibration solutions and saved them in the tables of multiple extensions, we need to apply them to the actual data. The | Now that we have derived all the calibration solutions and saved them in the tables of multiple extensions, we need to apply them to the actual data. The '''[https://casadocs.readthedocs.io/en/v6.4.1/api/tt/casatasks.calibration.applycal.html?highlight=applycal applycal]''' task commands will apply the solution tables to the DATA and write a new column CORRECTED_DATA as it is standard for CASA. Important: make sure you set <tt>parang=True</tt>. | ||
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Next, we will '''[https://casadocs.readthedocs.io/en/v6.4.1/api/tt/casatasks.manipulation.split.html?highlight=split split]''' the corrected (i.e., calibrated) Jupiter target data from the MS we started with and write it to a new single-source MS. | |||
<source lang="python"> | <source lang="python"> | ||
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</source> | </source> | ||
You can use | You can use '''[https://casadocs.readthedocs.io/en/v6.4.1/api/tt/casaplotms.plotms.html?highlight=plotms plotms]''' task to look at the split calibrated data. | ||
== Initial imaging (Stokes I) == | == Initial imaging (Stokes I) == | ||
Revision as of 18:17, 14 December 2022
| DISCLAIMER |
| This is an advanced reference guide to calibration and imaging of pre-upgrade VLA polarimetric data with CASA 5.5.0. If you are a beginning or novice user, please consult relevant CASA guides first. |
Data Import
This CASA guide discusses how to set the flux scale for calibration of an archival VLA 6cm data set taken in 1999. The original observation included several planets, among them was Jupiter, which will be the focus of this guide. This observation was taken in D-configuration, with a resolution of around 14 arcsec.
The data set for this tutorial can be downloaded from this link: planets_6cm.fits (129MB).
Import the data into CASA. Task importuvfits will read the original AIPS friendly UVFITS format and create a CASA native MS.
importuvfits(fitsfile='planets_6cm.fits', vis='jupiter6cm.demo.ms', antnamescheme='old')
Use listobs to check the observation setup and print verbose summary of the observations to the CASA logger.
listobs(vis='jupiter6cm.demo.ms')
The output of this task is fairly long, the abridged version is shown below since we may need some of this information later on during our calibration.
########################################## ##### Begin Task: listobs ##### Observer: FLUX99 Project: Observation: VLA Computing scan and subscan properties... Data records: 2021424 Total elapsed time = 85136.5 seconds Observed from 15-Apr-1999/23:15:25.0 to 16-Apr-1999/22:54:21.6 (TAI) [...] Fields: 13 ID Code Name RA Decl Epoch SrcId nRows 0 A 0137+331 01:37:41.299500 +33.09.35.13400 J2000 0 72946 1 T 0813+482 08:13:36.051800 +48.13.02.26200 J2000 1 227524 2 A 0542+498 05:42:36.137900 +49.51.07.23400 J2000 2 227058 3 T 0437+296 04:37:04.174700 +29.40.15.13600 J2000 3 113424 4 VENUS 04:06:54.109428 +22.30.35.90609 J2000 4 121098 5 A 0521+166 05:21:09.886000 +16.38.22.05200 J2000 5 81258 6 T 1411+522 14:11:20.647700 +52.12.09.14100 J2000 6 243608 7 A 1331+305 13:31:08.288100 +30.30.32.96000 J2000 7 307958 8 MARS 14:21:41.365747 -12.21.49.45444 J2000 8 118570 9 NGC7027 21:07:01.593000 +42.14.10.18600 J2000 9 136082 10 NEPTUNE 20:26:01.136316 -18.54.54.21127 J2000 10 157736 11 URANUS 21:15:42.828572 -16.35.05.59272 J2000 11 99412 12 JUPITER 00:55:34.043951 +04.45.44.70633 J2000 12 114750 Spectral Windows: (2 unique spectral windows and 1 unique polarization setups) SpwID Name #Chans Frame Ch0(MHz) ChanWid(kHz) TotBW(kHz) CtrFreq(MHz) Corrs 0 none 1 TOPO 4885.100 50000.000 50000.0 4885.1000 RR RL LR LL 1 none 1 TOPO 4835.100 50000.000 50000.0 4835.1000 RR RL LR LL Sources: 26 ID Name SpwId RestFreq(MHz) SysVel(km/s) 0 0137+331 0 0 0 0 0137+331 1 0 0 1 0813+482 0 0 0 1 0813+482 1 0 0 2 0542+498 0 0 0 2 0542+498 1 0 0 3 0437+296 0 0 0 3 0437+296 1 0 0 4 VENUS 0 0 0 4 VENUS 1 0 0 5 0521+166 0 0 0 5 0521+166 1 0 0 6 1411+522 0 0 0 6 1411+522 1 0 0 7 1331+305 0 0 0 7 1331+305 1 0 0 8 MARS 0 0 0 8 MARS 1 0 0 9 NGC7027 0 0 0 9 NGC7027 1 0 0 10 NEPTUNE 0 0 0 10 NEPTUNE 1 0 0 11 URANUS 0 0 0 11 URANUS 1 0 0 12 JUPITER 0 0 0 12 JUPITER 1 0 0 Antennas 27 [....] ##### End Task: listobs ##### ##########################################
Next use plotants to check the array configuration and select a reference antenna. Here, we will use antenna '11' as a reference since it's located in the middle of the array.
plotants(vis='jupiter6cm.demo.ms', figfile='jupiter6cm.demo.ant.png')
Note (for uvfits sourced directly from archive only): CASA 5.4 and earlier versions will not plot the antennas properly. This is to be resolved in future CASA versions. If this occurs then a reference antenna can be selected using the listobs task and choosing an antenna located on a pad close to the center of the array (Pads numbers increase with distance from the center of the array, ie. "VLA:_N1" and "EVLA:W2" are pads close to the center of the array, where as, "VLA:_N18" is not).
Data Inspection and Flagging
In this section we present two methods of flagging the data:
- Interactive flagging using plotms, which is destructive to the data set and cannot be undone. If a mistake is made, you must start over with a new copy of the data set. Because of the destructive nature of this method, it is generally not recommended.
- Non-interactive flagging using flagdata, which is not destructive to the data set and can be undone (be sure to set flagbackup=True). If a mistake is made, you may undo the flagged data. This is the recommended approach to flagging any data set, new (JVLA) or old (VLA).
For either method (interactive and non-interactive flagging), we will use plotms to inspect the data.
plotms(vis='jupiter6cm.demo.ms', selectdata=True, field='1331+305', correlation='RR,LL', xaxis='uvdist', yaxis='amp')
Inspect the primary flux density scale and polarization angle calibrator, 1331+305 (3C286). Inspect RR,LL and RL,LR correlations separately due to large amplitude differences between them (when all correlations are plotted together, the RL,LR will seem like bad data due to their much lower amplitudes as compared to RR,LL).
Interactive Flagging
- Use Mark Regions within the plotms GUI to draw boxes around points to flag, and hit Flag to flag.
Now, inspect the other two sources we are interested in, the polarization leakage calibrator (0137+331) and our target source (JUPITER).
Non-Interactive Flagging
- Use plotms to inspect the data set and flagdata to flag the data. While inspecting the data, you may notice that Antenna 9 (ID=8) in spw='1' is often bad. The bad data on Antenna 9 are in the last 4 scans in spw='1' for the 0137+331 calibrator and for the target source (JUPITER), as well as in the last scan for all antennas in both spws on the target source. We can flag these points with the following flagdata task executions.
flagdata(vis='jupiter6cm.demo.ms', mode='manual', field='0137+331', spw='1', antenna='9', timerange='42:00:00~48:00:00', flagbackup=True)
flagdata(vis='jupiter6cm.demo.ms', mode='manual', field='JUPITER', spw='1', antenna='9', timerange='16:26:00~22:20:00', flagbackup=True)
flagdata(vis='jupiter6cm.demo.ms', mode='manual', field='JUPITER', spw='', timerange='21:40:00~22:20:00', flagbackup=True)
- There are more data points to flag -- keep flagging until you are happy with the results. The following commands will get rid of most bad data, but depending on how clean the data you want to proceed with, you may still want to inspect them in plotms and flag interactively the remainder of bad data points.
flagdata(vis='jupiter6cm.demo.ms',mode='clip',field='1331+305',correlation='ABS_RR,LL',clipoutside=False,clipminmax=[0,0.75], flagbackup=True)
flagdata(vis='jupiter6cm.demo.ms',mode='clip',field='1331+305',correlation='ABS_RL,LR',clipoutside=False,clipminmax=[0,0.04], flagbackup=True)
flagdata(vis='jupiter6cm.demo.ms',mode='clip',field='0137+331',correlation='ABS_RR,LL',clipoutside=False,clipminmax=[0,0.55], flagbackup=True)
flagdata(vis='jupiter6cm.demo.ms',mode='clip',field='0137+331',correlation='ABS_RL,LR',clipoutside=False,clipminmax=[0,0.01], flagbackup=True)
If you are unfamiliar with flagging in CASA, consult the detailed topical guide Flagging VLA Data.
Calibration
Flux Density Scale
Next we will use setjy to set the absolute flux density scale, only for Stokes I at the moment (the total flux density model).
- Our primary flux calibrator here is 1331+305 (3C286).
- The default model for CASA 5.5+ is 'Perley-Butler 2017'.
setjy(vis='jupiter6cm.demo.ms', field='1331+305', model='3C286_C.im')
Initial Gain Calibration
At this stage the data have an overall flux density scaling determined, but full gain solutions aren't there yet. The relevant task is gaincal (analogous to the AIPS task CALIB). Gaincal will produce a separate table with solutions, and we will use appropriate extensions to keep track of the different tables and their corresponding solutions (e.g., gain curve table = .gc).
NOTE: Since we have only two single-channel continuum spw, we do not want to do bandpass calibration nor solve for delays within spws as is currently done with wide bandwidth JVLA data.
First, generate an antenna zenith-angle dependent VLA gain curve calibration table.
gencal(vis='jupiter6cm.demo.ms', caltable='jupiter6cm.demo.gc', caltype='gc')
Now, solve for antenna gains on 1331+305 and 0137+331, using the generated gain curve table (.gc).
gaincal(vis='jupiter6cm.demo.ms', caltable='jupiter6cm.demo.G', field='1331+305,0137+331', spw='', gaintype='G', calmode='ap', solint='inf', combine='', refant='11', minsnr=3, gaintable=['jupiter6cm.demo.gc'], parang=False)
# And check the solutions
plotms(vis='jupiter6cm.demo.G', xaxis='time', yaxis='amp', gridrows=3, gridcols=3, iteraxis='antenna')
plotms(vis='jupiter6cm.demo.G', xaxis='time', yaxis='phase', plotrange=[-1,-1,-200,200], gridrows=3, gridcols=3, iteraxis='antenna')
If all looks good, bootstrap the flux density scale of the flux calibrator onto the phase calibrators (CASA's fluxscale task is equivalent to GETJY in AIPS). When executing fluxscale, the calibration table with the extension .G is modified and stored as a new table with the extension .Gflx.
myFluxscale = fluxscale(vis='jupiter6cm.demo.ms', caltable='jupiter6cm.demo.G', fluxtable='jupiter6cm.demo.Gflx', reference='1331+305', transfer='0137+331', incremental=True, append=False, display=False)
The output is displayed in the logger as well as stored in the myFluxscale python dictionary.
Beginning fluxscale--(MSSelection version)------- Found reference field(s): 1331+305 Found transfer field(s): 0137+331 Flux density for 0137+331 in SpW=0 (freq=4.8851e+09 Hz) is: 5.29665 +/- 0.00449217 (SNR = 1179.09, N = 54) Flux density for 0137+331 in SpW=1 (freq=4.8351e+09 Hz) is: 5.34890 +/- 0.00176819 (SNR = 3025.07, N = 54) Fitted spectrum for 0137+331 with fitorder=1: Flux density = 5.32271 +/- 1.70229e-07 (freq=4.86004 GHz) spidx=-0.954124 (degenerate) Storing result in jupiter6cm.demo.Gflx Writing solutions to table: jupiter6cm.demo.Gflx
Before proceeding, inspect the flux density calibration and save results to a file.
plotms(vis='jupiter6cm.demo.Gflx', xaxis='time', yaxis='amp', showgui=True, plotfile='jupiter6cm.demo.Gflx.amp.png')
plotms(vis='jupiter6cm.demo.Gflx', xaxis='time', yaxis='phase', plotrange=[-1,-1,-200,200], showgui=True, plotfile='jupiter6cm.demo.Gflx.phase.png')
Polarization Calibration
Just as in the step of the initial gain calibration, since our old VLA data have single-channel continuum spws, we do not want to solve for KCROSS delays in our polarization calibration. Instead, we directly solve for D and X terms.
Set the Polarization Model
First, set the polarization model for the polarized position-angle calibrator (here 1331+305=3C286 which is also our primary flux calibrator). For polarization properties of your primary polarization calibrator see the Polarimetry section of the VLA Observing Guide.
i0=7.3109 # Stokes I value for spw 0 ch 0
f0=4.8851 # Frequency for spw0 ch0 (note that in our data the 'lower' spw is actually higher frequency)
alpha=log(i0/7.35974932)/log(4.8351/f0) # Values from our setjy() run on Stokes I earlier
c0=0.114 # Fractional polarisation 11.4% for 5GHz
d0=33*pi/180 # Polarization angle 33deg in radians
myPolSetjy = setjy(vis='jupiter6cm.demo.ms', field='1331+305', standard='manual', spw='', fluxdensity=[i0,0,0,0], spix=[alpha,0], reffreq=str(f0)+'GHz', polindex=[c0,0], polangle=[d0,0], scalebychan=True, usescratch=False)
The results are displayed in the CASA logger as well as saved in the myPolSetjy python dictionary
#In CASA
CASA <49>: myPolSetjy
Out[49]:
{'7': {'0': {'fluxd': array([ 7.3109 , 0.33899165, 0.7613877 , 0. ])},
'1': {'fluxd': array([ 7.26237491, 0.33674164, 0.7563341 , 0. ])},
'fieldName': '1331+305'},
'format': "{field Id: {spw Id: {fluxd: [I,Q,U,V] in Jy}, 'fieldName':field name }}"}
Solve for the Leakage Terms (D terms)
Solve for polarization leakage on 0137+331. In this step we solve for the instrumental polarization. We will assume here our calibrator has unknown polarization (poltype='D+QU' if good parallactic coverage, otherwise poltype='D', consult polcal for more information on options).
polcal(vis='jupiter6cm.demo.ms', caltable='jupiter6cm.demo.D', field='0137+331', spw='', refant='11', poltype='D+QU', solint='inf', combine='scan',minsnr=3, gaintable=['jupiter6cm.demo.gc', 'jupiter6cm.demo.G'], gainfield=['','0137+331',''])
Check the solutions
plotms(vis='jupiter6cm.demo.D', xaxis='antenna', yaxis='amp', showgui=True, plotfile='jupiter6cm.demo.D.amp.png')
plotms(vis='jupiter6cm.demo.D', xaxis='antenna', yaxis='phase', plotrange=[-1,-1,-200,200], showgui=True, plotfile='jupiter6cm.demo.D.phase.png')
plotms(vis='jupiter6cm.demo.D', xaxis='antenna', yaxis='snr', showgui=True, plotfile='jupiter6cm.demo.D.snr.png')
Solve for the R-L Polarization angle (X term)
The total polarization is now correct (since we just calibrated the instrumental polarization, i.e., D terms). Now the R-L phase needs to be calibrated to obtain an accurate polarization position angle.
polcal(vis='jupiter6cm.demo.ms', caltable='jupiter6cm.demo.X', field='1331+305', spw='', refant='11', poltype='Xf', solint='inf', combine='scan',minsnr=3, gaintable=['jupiter6cm.demo.gc', 'jupiter6cm.demo.G', 'jupiter6cm.demo.D'], gainfield=['','1331+305','',''])
Check the solutions in the CASA logger window
The following calibration term is arranged for solve: . Xf Jones: table=jupiter6cm.demo.X append=false solint=inf,none refantmode='flex' refant='none' minsnr=3 apmode=AP solnorm=false For solint = inf, found 2 solution intervals. Mean position angle offset solution for 1331+305 (spw = 0) = 80.7525 deg. Mean position angle offset solution for 1331+305 (spw = 1) = 48.9853 deg. Found good Xf Jones solutions in 2 solution intervals.
NOTE: If you are using CASA 4.7 or earlier, you may want to use poltype='X' in X-term calculations (Mueller matrices). For CASA 5.0 and later this option will not work (the relevant CASA documentation is being updated), and hence you need to use poltype='Xf' (Jones matrices). Although 'Xf' should be used predominantly for large bandwidths, which clearly is not the case here, it can also be used for the single channel old VLA data as long as you make sure the interp parameter is set to default (which should be nearest).
Apply the Calibration
Now that we have derived all the calibration solutions and saved them in the tables of multiple extensions, we need to apply them to the actual data. The applycal task commands will apply the solution tables to the DATA and write a new column CORRECTED_DATA as it is standard for CASA. Important: make sure you set parang=True.
applycal(vis='jupiter6cm.demo.ms', field='1331+305', spw='', selectdata=False, gaintable=['jupiter6cm.demo.gc', 'jupiter6cm.demo.G', 'jupiter6cm.demo.D','jupiter6cm.demo.X'], gainfield=['','1331+305'], calwt=[False], parang=True)
applycal(vis='jupiter6cm.demo.ms', field='0137+331', spw='', selectdata=False, gaintable=['jupiter6cm.demo.gc', 'jupiter6cm.demo.G', 'jupiter6cm.demo.Gflx','jupiter6cm.demo.D','jupiter6cm.demo.X'], gainfield=['','0137+331','0137+331'], calwt=[False], parang=True)
applycal(vis='jupiter6cm.demo.ms', field='JUPITER', spw='', selectdata=False, gaintable=['jupiter6cm.demo.gc', 'jupiter6cm.demo.G', 'jupiter6cm.demo.Gflx','jupiter6cm.demo.D','jupiter6cm.demo.X'], gainfield=['','0137+331','0137+331'], calwt=[False], parang=True)
Next, we will split the corrected (i.e., calibrated) Jupiter target data from the MS we started with and write it to a new single-source MS.
split(vis='jupiter6cm.demo.ms', outputvis='jupiter6cm.demo.JUPITER.split.ms', field='JUPITER', datacolumn='corrected')
You can use plotms task to look at the split calibrated data.
Initial imaging (Stokes I)
We will now image and clean the calibrated Jupiter data. In the next step we will perform self-calibration, so here in the initial imaging we will not clean too deeply and we will also save the model in the MS data (with the use of parameter savemodel in tclean()).
Since we set mask="" in our cleaning tasks, the interactive GUI will not allow you to do the deconvolution before you draw the mask on at least one plane. When drawing a mask, make sure to extend it to all channels and all polarisations.
tclean(vis='jupiter6cm.demo.JUPITER.split.ms', stokes='I', field='', spw='', imagename='jupiter6cm.demo.JUPITER.I.clean1', robust = 0.0, imsize=[288], cell=['3arcsec'], specmode='mfs', deconvolver='hogbom', weighting='briggs', threshold='0.1mJy', mask='', niter=500, interactive=True, cycleniter=100, savemodel='modelcolumn', pblimit=-0.2)
Inspect the quality of the cleaned images with imstat().
imstat(imagename='jupiter6cm.demo.JUPITER.I.clean1.image', stokes='I', box='216,1,287,72')
In this initial imaging the deconvolution will stop with the iteration limit since we set it fairly low. We 'cleaned' approximately 4.3 Jy in this initial imaging step, and reached rms of about 3.52 mJy/bm.
Self-calibration
In the self calibration step we run gaincal() that will make use of the newly created MODEL column in our MS file.
gaincal(vis='jupiter6cm.demo.JUPITER.split.ms', caltable='jupiter6cm.demo.JUPITER.split.selfcal1', field='', spw='', gaintype='G', calmode='p', solint='30s', combine='', refant='11', parang=False, append=False, selectdata=False)
Inspect the solutions
plotms(vis='jupiter6cm.demo.JUPITER.split.selfcal1',xaxis='time',yaxis='amp',gridrows=2, gridcols=3, iteraxis='antenna')
plotms(vis='jupiter6cm.demo.JUPITER.split.selfcal1',xaxis='time',yaxis='phase', gridrows=2, gridcols=3 ,iteraxis='antenna',plotrange=[-1,-1,-180,180])
And apply the calibration to the DATA(creating a CORRECTED column in the MS)
applycal(vis='jupiter6cm.demo.JUPITER.split.ms', field='', spw='', selectdata=False, gaintable=['jupiter6cm.demo.JUPITER.split.selfcal1'], gainfield=[''], interp=['nearest'],calwt=[False], applymode='calflag')
Now, image the self-calibrated data
tclean(vis='jupiter6cm.demo.JUPITER.split.ms', stokes='I', field='', spw='', imagename='jupiter6cm.demo.JUPITER.I.clean2', robust= 0.0, imsize=[288], cell=['3arcsec'], specmode='mfs', deconvolver='hogbom', weighting='briggs', threshold='0.05mJy', mask='', niter=10000, interactive=True, cycleniter=100, pblimit=-0.2)
Check the image statistics
imstat(imagename='jupiter6cm.demo.JUPITER.I.clean2.image', stokes='I', box='216,1,287,72')
After one cycle of self-calibration with tclean() we reached rms=1.10 mJy/bm. But bear in mind that the rms values may differ for you since they will depend on how deeply you cleaned and how good a mask you applied.
Full Stokes Imaging
At this stage we will perform full Stokes imaging to create image of each Stokes parameter that we will later use to create polarised intensity and angle images.
tclean(vis='jupiter6cm.demo.JUPITER.split.ms', stokes='IQUV', field='', spw='', imagename='jupiter6cm.demo.JUPITER.IQUV.clean', robust= 0.0, imsize=[288], cell=['3arcsec'], specmode='mfs', deconvolver='clarkstokes', weighting='briggs', threshold='0.05mJy', mask='', niter=10000, interactive=True, cycleniter=100, pblimit=-0.2)
Inspect the quality of the cleaned images with imstat() (do it for each Stokes separately, as otherwise imstat() will return an average of all Stokes). You should be reaching values of about 1.1 mJy/bm (I), 0.62 mJy/bm (Q), 0.90 mJy/bm (U), 0.16 mJy/bm (V).
Polarisation Intensity and Position Angle Images
We now want to save each Stokes plane as separate images. We can use either the imsubimage() or immath() tasks to do so.
Run
imsubimage(imagename='jupiter6cm.demo.JUPITER.IQUV.clean.image',outfile='JUPITER.I.image',stokes='I')
imsubimage(imagename='jupiter6cm.demo.JUPITER.IQUV.clean.image',outfile='JUPITER.Q.image',stokes='Q')
imsubimage(imagename='jupiter6cm.demo.JUPITER.IQUV.clean.image',outfile='JUPITER.U.image',stokes='U')
or
immath(imagename='jupiter6cm.demo.JUPITER.IQUV.clean.image', mode='evalexpr', stokes='I', expr='IM0', outfile='JUPITER.I.image')
immath(imagename='jupiter6cm.demo.JUPITER.IQUV.clean.image', mode='evalexpr', stokes='Q', expr='IM0', outfile='JUPITER.Q.image')
immath(imagename='jupiter6cm.demo.JUPITER.IQUV.clean.image', mode='evalexpr', stokes='U', expr='IM0', outfile='JUPITER.U.image')
Finally, we want to create the polarization intensity (POLI) and position angle (POLA) images.
immath(imagename=['JUPITER.Q.image','JUPITER.U.image'], mode='poli', outfile='JUPITER.POLI.image')
We will now use the polithresh parameter when creating the polarisation angle image to get rid of the noise. First check the statistic in the POLI image, and then use it as a threshold while creating the POLA image (in the example below equal to 4 sigma).
imstat(imagename='JUPITER.POLI.image', box='216,1,287,72')
immath(imagename=['JUPITER.Q.image','JUPITER.U.image'], mode='pola', outfile='JUPITER.POLA.image',polithresh='4.5mJy/beam')
Again, check the statistics of these final images with imstat() and/or viewer().
And that's it. For the tutorial on how to perform analysis, display and manipulation of the polarisation images now, consult the appropriate VLA CASA guides.
