SSSC6 PURR Logs

Stewart Gleadow, gleadows@unimelb.edu.au, University of Melbourne

Using calico-view-ms.py

View visibility data for some baselines, just to to a quick sanity check on the MS, see that it contains data that resembles that expected.

Create a dirty image of the uncalibrated data, check that it looks like there is a source convolved with the PSF of WSRT in the centre of the beam in Stokes I and Q, but not in U and V.

Averaging all freq channels into one to keep file sizes small.

Using calico-wsrt.py

Set compile options to calibrate G-Jones on visibilities, and subtract LSM, shown in image below.

Pre-load the bookmark for inspector:G, so that we can see the gain solutions. Expect them to be varying perioically in amplitude but flat in phase, as shown below.

Run the script to calibrate G diagonal terms, shown in image below.

Now that we have calibrated the gains, image the residuals from LSM (again using calico-wsrt.py).

Average all frequency channels together, since we know the gain solution is the same for all channels, and to keep file size down (see runtime settings below).

Expect to see nano Jy level noise remaing in Stokes I and Q, indicating that the model has been accurately removed and the calibration successful, and nothing in Stokes U and V as there was never any signal in those channels, and we have not included any instrumental leakage.