EVLA high frequency spectral line tutorial - IRC+10216 - calibration: Difference between revisions

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Create a plot of antenna positions using {{plotants}}.
Create a plot of antenna positions using {{plotants}}.
[[Image:elevationvstime.png|thumb|Elevation as a function of time (after selecting colorize by field).]]

<source lang="python">
<source lang="python">

Revision as of 16:56, 6 January 2012

This page is under development

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.


VLT V-band image of IRC+10216 showing dust rings out to a radius of 90" by Leão et al. (2006, A&A, 455, 187).

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.

For example,

wget 'ftp://ftp.aoc.nrao.edu/staff/gvanmoor/community_day/*'

Initial Inspection and Flagging

GEt a summary listing of the data set using listobs.

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 + J2000   2     32726
  3    NONE IRC+10216           09:47:57.38200 + J2000   3     99540
  5    F    J1229+0203          12:29:06.69973 + J2000   5     5436
  7    E    J1331+3030          13:31:08.28798 + 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   -  +
  1    ea02  E02       25.0 m   -  +
  2    ea03  E09       25.0 m   -  +
  3    ea04  W01       25.0 m   -  +
  4    ea05  W08       25.0 m   -  +
  5    ea07  N06       25.0 m   -  +
  6    ea08  N01       25.0 m   -  +
  7    ea09  E06       25.0 m   -  +
  8    ea12  E08       25.0 m   -  +
  9    ea15  W06       25.0 m   -  +
  10   ea19  W04       25.0 m   -  +
  11   ea20  N05       25.0 m   -  +
  12   ea21  E01       25.0 m   -  +
  13   ea22  N04       25.0 m   -  +
  14   ea23  E07       25.0 m   -  +
  15   ea24  W05       25.0 m   -  +
  16   ea25  N02       25.0 m   -  +
  17   ea27  E03       25.0 m   -  +
  18   ea28  N08       25.0 m   -  +

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
Antenna locations from running plotants

Create a plot of antenna positions using plotants.

Result of plotms
Zooming in and marking region (hatched box)

Next, let's look at all the source amplitudes as a function of time using plotms.

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.


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.


There is no Ka-band model of 3C286. We will use the K-band model instead.


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.

Bandpass Calibration

Correct the phase variations with time before solving for the bandpass to prevent decorrelation of the vector averaged bandpass solution.

Phase only calibration before bandpass. The 4 lines are both polarizations in both spw, unfortunately two of them get the same color green at the moment.
gaincal(vis=vis, caltable='bpphase.gcal', field='5', spw='0~1:20~40',
        refant='ea02', gaintype='G', calmode='p',solint='int',

Plot the solutions using plotcal.


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').

bandpass(vis=vis, caltable='bandpass.bcal', field='5', refant='ea02',
         solint='inf', solnorm=T, gaintable='bpphase.gcal',

Plot the solutions, amplitude and phase:

Amplitude Bandpass solutions
Phase Bandpass solutions


Remaining Calibration

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

  1. doing a phase only calibration on all calibrators using gaincal,
  2. doing amplitude only calibration on all calibrators while applying the phase-only solutions, and
  3. 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.


--Crystal Brogan --additions: Juergen Ott

Last checked on CASA Version 3.3.0.