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Titolo:
PHASE-REFERENCED VISIBILITY AVERAGING IN OPTICAL LONG-BASE-LINE INTERFEROMETRY
Autore:
QUIRRENBACH A; MOZURKEWICH D; BUSCHER DF; HUMMEL CA; ARMSTRONG JT;
Indirizzi:
MAX PLANCK INST EXTRATERR PHYS,GIESSENBACHSTR D-85748 GARCHING GERMANY USN OBSERV,NRL USNO OPT INTERFEROMETER PROJECT WASHINGTON DC 20392 UNIV SPACE RES ASSOC WASHINGTON DC 20024 USN,RES LAB,DIV REMOTE SENSING WASHINGTON DC 20375
Titolo Testata:
Astronomy and astrophysics
fascicolo: 3, volume: 286, anno: 1994,
pagine: 1019 - 1027
SICI:
0004-6361(1994)286:3<1019:PVAIOL>2.0.ZU;2-5
Fonte:
ISI
Lingua:
ENG
Soggetto:
III STELLAR INTERFEROMETER; ASTROMETRY;
Keywords:
ATMOSPHERIC EFFECTS; INSTRUMENTATION, INTERFEROMETERS; METHODS, OBSERVATIONAL; METHODS, DATA ANALYSIS; TECHNIQUES, INTERFEROMETRIC;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
14
Recensione:
Indirizzi per estratti:
Citazione:
A. Quirrenbach et al., "PHASE-REFERENCED VISIBILITY AVERAGING IN OPTICAL LONG-BASE-LINE INTERFEROMETRY", Astronomy and astrophysics, 286(3), 1994, pp. 1019-1027

Abstract

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 largezenith angles is the most important limitation. Tests with MkIII datain 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 a Boo close to the first null of the visibility function to show that the MkIII data are free from additive bias at the V2 less-than-or-equal-to 10(-4) level. The absence of any bias larger than this value is an important requirement for future imaging interferometers.

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Documento generato il 25/11/20 alle ore 04:31:14