EVLA high frequency spectral line tutorial - IRC+10216 - calibration
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This CASA Guide provides a simplified approach to the editing, calibration, and imaging of a galactic EVLA observation for use in NRAO Community Day Events. For a complete description of the data reduction process see EVLA high frequency Spectral Line tutorial - IRC+10216 part1 and EVLA high frequency Spectral Line tutorial - IRC+10216 part2.
This tutorial describes the data reduction for two spectral lines, HC3N and SiS, observed toward the AGB star IRC+10216 by the EVLA in D-configuration.
Getting the data
The data for this tutorial can be obtained by anonymous FTP from ftp://ftp.aoc.nrao.edu/staff/gvanmoor/community_day/. Download all 4 TAR files.
# In UNIX wget 'ftp://ftp.aoc.nrao.edu/staff/gvanmoor/community_day/*'
Initial Inspection and Flagging
GEt a summary listing of the data set using listobs.
# In CASA vis = 'day2_TDEM0003_20s_full' listobs(vis=vis, verbose=True)
Below we have cut and pasted the most relevant output from the logger.
Fields: 4 ID Code Name RA Decl Epoch SrcId nVis 2 D J0954+1743 09:54:56.82363 +184.108.40.2064 J2000 2 32726 3 NONE IRC+10216 09:47:57.38200 +220.127.116.1100 J2000 3 99540 5 F J1229+0203 12:29:06.69973 +02.03.08.5982 J2000 5 5436 7 E J1331+3030 13:31:08.28798 +18.104.22.16889 J2000 7 2736 (nVis = Total number of time/baseline visibilities per field) Spectral Windows: (2 unique spectral windows and 1 unique polarization setups) SpwID #Chans Frame Ch1(MHz) ChanWid(kHz) TotBW(kHz) Corrs 0 64 TOPO 36387.2295 125 8000 RR RL LR LL 1 64 TOPO 36304.542 125 8000 RR RL LR LL Sources: 10 ID Name SpwId RestFreq(MHz) SysVel(km/s) 0 J1008+0730 0 0.03639232 -0.026 0 J1008+0730 1 0.03639232 -0.026 2 J0954+1743 0 0.03639232 -0.026 2 J0954+1743 1 0.03639232 -0.026 3 IRC+10216 0 0.03639232 -0.026 3 IRC+10216 1 0.03639232 -0.026 5 J1229+0203 0 0.03639232 -0.026 5 J1229+0203 1 0.03639232 -0.026 7 J1331+3030 0 0.03639232 -0.026 7 J1331+3030 1 0.03639232 -0.026 Antennas: 19: ID Name Station Diam. Long. Lat. 0 ea01 W09 25.0 m -22.214.171.124 +126.96.36.199 1 ea02 E02 25.0 m -107.37.04.4 +33.54.01.1 2 ea03 E09 25.0 m -188.8.131.52 +184.108.40.206 3 ea04 W01 25.0 m -107.37.05.9 +33.54.00.5 4 ea05 W08 25.0 m -220.127.116.11 +18.104.22.168 5 ea07 N06 25.0 m -107.37.06.9 +22.214.171.124 6 ea08 N01 25.0 m -107.37.06.0 +33.54.01.8 7 ea09 E06 25.0 m -126.96.36.199 +188.8.131.52 8 ea12 E08 25.0 m -184.108.40.206 +220.127.116.11 9 ea15 W06 25.0 m -18.104.22.168 +22.214.171.124 10 ea19 W04 25.0 m -126.96.36.199 +188.8.131.52 11 ea20 N05 25.0 m -107.37.06.7 +33.54.08.0 12 ea21 E01 25.0 m -107.37.05.7 +184.108.40.206 13 ea22 N04 25.0 m -107.37.06.5 +33.54.06.1 14 ea23 E07 25.0 m -220.127.116.11 +18.104.22.168 15 ea24 W05 25.0 m -22.214.171.124 +126.96.36.199 16 ea25 N02 25.0 m -107.37.06.2 +33.54.03.5 17 ea27 E03 25.0 m -107.37.02.8 +33.54.00.5 18 ea28 N08 25.0 m -107.37.07.5 +188.8.131.52
We summarize the observing strategy in this table.
|Gain calibrator||J0954+1743||field id = 2|
|Bandpass calibrator||J1229+0203||field id = 5|
|Flux calibrator||J1331+3030 (3C286)||field id = 7|
|Science target||IRC+10216||field id = 3|
Create a plot of antenna positions using plotants.
# In CASA plotants(vis=vis)
Next, let's look at all the source amplitudes as a function of time using plotms.
# In CASA plotms(vis=vis, xaxis='time', yaxis='amp', correlation='RR,LL', avgchannel='64', spw='0:4~60', coloraxis='field')
Now zoom in on the region very near zero amplitude for sources J0954+1743 and IRC+10216. To zoom, select the Zoom tool in lower left corner of the plotms GUI, then you can left click to draw a box. Look for the low values (you may want to zoom a few times to really see the suspect points clearly). Now use the Mark Region and Locate buttons (located along the bottom of the GUI) to see which antenna is causing problems. The output will be shown in the logger. Since all the "located" baselines include ea12, this is the responsible antenna.
Now click the clear region button, and then go back to the zoom button to zoom in further to note exactly what the time range is: 03:41:00~04:10:00.
Check the other sideband by changing spw to 1:4~60. You will have to rezoom. If you have trouble, click on the Mark icon and then back to zoom. In spw=1, ea07 is bad from the beginning until after next pointing run: 03:21:40~04:10:00. To see this, compare the amplitudes when antenna is set to 'ea07' and when it is set to one of the other antennas, such as 'ea08'.
If you set antenna to 'ea12' and zoom in on this intial timerange, you can also see that ea12 is bad during the same time range as for spw 0. You can also see this by entering '!ea07' for antenna, which removes ea07 from the plot (in CASA selection, ! deselects).
We can flag the bad data using flagdata.
# In CASA flagdata(vis=vis, field=['2,3','2,3'], spw=['','1'], antenna=['ea12','ea07'], timerange=['03:41:00~04:10:00','03:21:40~04:10:00'])
flagdata works by spanning up a matrix. The first entries in each list must be taken as one flagging command, as well as the second entries etc. Lists within lists are fine. In the above example, the first flagging command is issued for fields 2 and 3 for all spws and within the 03:41:00~04:10:00 timerange. A second command is again for the fields 2 and 3 but for spw 1 only and for the second timerange in the list '03:21:40~04:10:00'.
Note that because the chosen timerange is limited to fields 2 and 3, the field parameter is not really needed; however, flagdata will run fastest if you put as many constraints as possible.
Set Up the Model for the Flux Calibrator
We set the model for the flux calibrator using setjy. First, check the availability of calibration models.
# In CASA setjy(vis=vis,listmodimages=T)
There is no Ka-band model of 3C286. We will use the K-band model instead.
# In CASA setjy(vis=vis,field='7',spw='0~1', modimage='3C286_K.im')
setjy scales the total flux in the model image to that appropriate for your individual spectral window frequencies according to the calibrator's flux and reports this number to the logger.
The logger output for each spw is: J1331+3030 (fld ind 7) spw 0 [I=1.7762, Q=0, U=0, V=0] Jy, (Perley-Butler 2010) J1331+3030 (fld ind 7) spw 1 [I=1.7794, Q=0, U=0, V=0] Jy, (Perley-Butler 2010)
The absolute fluxes for the frequencies have now been determined and one can proceed to the bandpass and complex gain calibrations.
Correct the phase variations with time before solving for the bandpass to prevent decorrelation of the vector averaged bandpass solution.
# In CASA gaincal(vis=vis, caltable='bpphase.gcal', field='5', spw='0~1:20~40', refant='ea02', gaintype='G', calmode='p',solint='int', gaincurve=T)
Plot the solutions using plotcal.
# In CASA plotcal(caltable='bpphase.gcal',xaxis='time',yaxis='phase', iteration='antenna',subplot=331,plotrange=[0,0,-180,180])
Next we can apply this phase solution on the fly while determining the bandpass solutions on the timescale of the bandpass calibrator scan (solint='inf').
# In CASA bandpass(vis=vis, caltable='bandpass.bcal', field='5', refant='ea02', solint='inf', solnorm=T, gaintable='bpphase.gcal', gaincurve=T)
Plot the solutions, amplitude and phase:
# In CASA plotcal(caltable='bandpass.bcal',xaxis='chan',yaxis='amp', iteration='antenna',subplot=331)
# In CASA plotcal(caltable='bandpass.bcal',xaxis='chan',yaxis='phase', iteration='antenna',subplot=331)
In this Community Day Event guide, we will skip over the remaining calibration steps. However, you can refer to EVLA high frequency Spectral Line tutorial - IRC+10216 part1 for full details. To summarize the missing steps, you bootstrap the flux densities of the secondary calibrators by
- doing a phase only calibration on all calibrators using gaincal,
- doing amplitude only calibration on all calibrators while applying the phase-only solutions, and
- deriving the flux density of the secondary calibrators while applying the previously obtained solutions.
Then, you can calibrate the target source using the phase and amplitude solutions you have obtained. Apply the target source calibration solutions using applycal. Use plotms to examine the calibrated data. If more flagging is required, redo all calibration steps. When the data look good, split the target source into a separate measurement set. Subtract the continuum flux using uvcontsub. Make Doppler corrections using cvel, or let clean do the Doppler corrections on the fly.
Last checked on CASA Version 3.3.0.