Phase-referenced visibility averaging in optical long-baseline interferometry

Details Phase-referenced visibility averaging in optical long-baseline interferometry Phase-referenced visibility averaging in optical long-baseline interferometry

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286.1019q&link_type=abstract

Astronomy and Astrophysics 286, 1019-1027 (1994)

Astronomy and Astrophysics

Astrophysics

17

Atmospheric Effects, Instrumentation: Interferometers, Methods: Observational, Methods: Data Analysis, Techniques: Interferometric

Scientific paper

In the photon-starved regime, the signal-to-noise ratio of interferometric data depends on the coherent integration time. To extend the integration time beyond the limit imposed by atmospheric fluctuations, the phases taken in a narrow "signal" channel can be corrected by referencing them to those taken in a wider "tracking" channel. A number of instrumental and atmospheric effects decorrelate the phases in the two channels and thus constrain the range of conditions under which the phase-referencing technique can be used. In the case of the MkIII stellar interferometer, differential refraction at intermediate to large zenith angles is the most important limitation. Tests with MkIII data in the photon-rich regime demonstrate that the phase-referencing technique works well at moderate zenith angles. In the photon-starved regime, the expected improvement of the signal-to-noise ratio is readily observed. We use phase-referenced data taken on the bright star αBoo close to the first null of the visibility function to show that the MkIII data are free from additive bias at the V^2^<=10^-4^ level. The absence of any bias larger than this value is an important requirement for future imaging interferometers.

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