3mm-VLBI : Detection Methods and Results

Details 3mm-VLBI : Detection Methods and Results 3mm-VLBI : Detection Methods and Results

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.5906d&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #59.06; Bulletin of the American Astronomical Society, Vol. 26, p.1413

Astronomy and Astrophysics

Astronomy

Scientific paper

In mm-VLBI observations, atmospheric turbulence and local oscillator phase noise often limit the coherence time to a few seconds. When such coherence losses severely limit the integration time, detection thresholds rise and weak sources cannot be detected. In April 1993 we observed a group of flat spectrum radio galaxies and quasars with a global 3mm network. Coherence problems in our data have led us to reformulate detection methods and measurements of visibility in terms of incoherent averages. These techniques are outlined with examples and results from high luminosity AGN observed during the 1993 campaign.

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