Note that the AIPS Cookbook is a useful general guide for calibration and imaging of VLBI data.
http://www.aips.nrao.edu/cook.html : AIPS Cookbook
Several documentations related the KaVA data analysis would be helpful.
For some parts of data analysis, KaVA would require special treatment as below :
2.1 Amplitude calibration
For amplitude calibration of KaVA data, KaVA provides the ANTAB files
to PIs. The ANTAB file contains the gain curves for each antenna,
and system temperature taken during the observation. You will obtain
the TY and GC tables, loading the ANTAB file by running the AIPS task
2.2 Parallactic angle correction
Time variation of a parallactic angle of a source occurs for the
receiving system mounted in an azimuth-elevation mounted telescope
and generates a phase rotation. This phase rotation can be corrected
with the AIPS task "CLCOR" with the adverb of OPCODE='PANG'.
In the case of VERA antenna, the field rotator in the receiving room
fixes the parallactic angle, and therefore it is not necessary to
run "CLCOR" for VERA antennas. But, you have to do this correction
for the KVN antennas.
2.3 Editing the AN table
The doppler velocity shifts due to the earth's rotation and its motion
within the solar system and towards the local standard of rest can be
corrected using the AIPS task "CVEL". When the ARRNAM keyword in the
AN table is "VLBA", then "CVEL" assumes that all data have been
fringe-rotated to the centre of the Earth and determine the velocity
correction accordingly. KaVA follows the VLBA and fringe rotates to the
Earth center. Thus, the ARRNAM keyword in the AN table has to be "VLBA".
Please run the task "TABED" and give "VLBA" to the ARRNAME keyword in
the AN table.
2.4 Gibbs ringing effects around a bright and narrow spectral line
KaVA contains comparatively-short baselines (~300 km) as a VLBI array,
and various Gibbs ringing effects could sometimes be seen in the case
of the bright narrow spectral features. It is strongly recommended to
smooth such spectral features when you correct the velocity shifts,
by running the AIPS task "CVEL" with the adverb of APARM(9)>1.
Figures : Water maser lines in Orion KL in the Tamna-Ulsan baseline
r10105a_bf_cvl: Before CVEL
r10105a_aft_cvl_nosmooth: After CVEL with APARM(9)=0 (no smoothing)
r10105a_aft_cvl_smooth: After CVEL with APARM(9)=2 (smoothing)