Blind operation of optical astronomical interferometers options and predicted performance

Details Blind operation of optical astronomical interferometers options and predicted performance Blind operation of optical astronomical interferometers options and predicted performance

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991exa.....2...57b&link_type=abstract

Experimental Astronomy (ISSN 0922-6435), vol. 2, no. 1, 1991, p. 57-71.

Physics

Optics

2

Adaptive Optics, Optical Paths, Particle Telescopes, Very Long Base Interferometry, Astrometry, Coherent Light, Mirrors

Scientific paper

Maximum sensitivity for optical interferometers is achieved only when the optical path lengths between the different arms can be equalized without using interference fringes on the research object itself. This is called 'blind operation' of the interferometer. This paper examines different options to achieve this, focusing on the application to the Very Large Telescope Interferometer (VLTI). It is proposed that blind operation should be done using a so-called coherence autoguider, working on an unresolved star of magnitude V = 11-13 within the isoplanatic patch for coherencing, which has a diameter of about 1 deg. Estimates of limiting magnitudes for the VLTI are also derived.

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