If you have followed the previous sections you should have ended up with a calibrated data set for all your sources (all of them stored in separated SPLIT files). Although the imaging process can be perfectly done within AIPS, as explained previously, Difmap allows you to perform a more dynamic imaging/calibration of the data. Its approach usually produces a easier way to perform the last and more refined steps in the calibration of an EVN dataset (basically flagging, imaging with different weightings, and self-calibration). For this reason, in this section we will describe how to improve the final EVN images by working with the data in both AIPS and Difmap and which steps will produce a better calibration on the target source. Although the tutorial is focused for phase-referencing observations, it can also be applied for other techniques.
This guide assumes that you have a small knowledge of how Difmap works. Otherwise, we recommend to follow a more detailed tutorial, as the one done by Doug Gobeille at Brandeis University. An exhaustive manual is also provided by ESO in this link (PS file), with a detailed explanation of all the tasks available in Difmap.
In the previous tutorial we have produced a standard calibration of your data by running fringe on your strongest sources, bandpass calibrating the data, and extrapolating the solutions to your target source. However, sometimes the obtained solutions are not optimal and some stations can exhibit a systematic offset in amplitude due to a wrong calibration (we remind you that in the EVN we have a wide variety of stations, with different capabilities, sizes, and sensitivities).
Because of that, we can improve the calibration if we self-calibrate the data using one strong source that has been observed regularly during the whole observation. In phase-referencing sessions this one should be the phase calibrator. Given that this source should be strong enough, close to our target source, and observed every few minutes, we can get much better solutions self-calibrating it and then extrapolating these solutions again to our target source. In those cases where your target source is bright enough, we can directly conduct this self-calibration directly on it, but in that case note that the absolute position of your source is lost (no astrometric studies can be performed).
The mentioned procedure will be carried out as follows:
During the last steps of the previous tutorial we exported the SPLIT files to the hard disk with FITTP. Hence we have the phase-calibrator data (calibrated) as a UVFITS file. We can then open Difmap and load these data into it (contrary to AIPS, Difmap works with the UVFITS files on the fly):
In Difmap there are several tasks to plot your data and interact with them. The most common ones are:
Once we have a dataset free of RFI