KVN and VERA Array

Calibrator Information

The NRAO VLBA calibrator survey is very useful to search for a continuum source which can be used as a reference source to carry out the delay, bandpass, and phase calibrations. The source list of this calibrator survey can be found at the following VLBA homepage,


http://www.vlba.nrao.edu/astro/calib/index.shtml.

For delay calibrations and bandpass calibrations, calibrators with 1 Jy or brighter are strongly recommended as listed in the VLBA fringe finder survey:


http://www.aoc.nrao.edu/~analysts/vlba/ffs.html.

Interval of observing calibrator scans must be shorter than 1 hour to track the delay and delay rate in the correlation process.

Figure 10: The receiver noise temperature (blue crosses) and the system noise temperature (red open circles) at the zenith in the K band and the Q band at the Mizusawa station.
\includegraphics[width=7cm]{fig-KaVA/fig10a.eps} \includegraphics[width=7cm]{fig-KaVA/fig10b.eps}


Figure 11: The zenith system noise temperature (red filled circles) at the K band (left) and the Q band (right) in the Ulsan station.
\includegraphics[width=15cm]{fig-KaVA/fig11.eps}



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KaVA ( KVN and VERA Array )