The VLT interferometer: Current status and expectations for the next 20 years

Details The VLT interferometer: Current status and expectations for the next 20 years The VLT interferometer: Current status and expectations for the next 20 years

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.354...91f&link_type=abstract

In ESA, Targets for Space-Based Interferometry p 91-98 (SEE N93-31750 12-89)

Astronomy and Astrophysics

Astronomy

2

Astronomical Interferometry, Interferometers, Telescopes, Arrays, Comparison, Planning, Space Observations (From Earth), Spaceborne Astronomy, Systems Engineering

Scientific paper

The layout, optical design and main components of the Very Large Telescope Interferometer (VLTI) are presented. VLTI subsystems are designed with sufficient flexibility to allow incorporation of new features later. Some parameters, which are of interest for a comparison between ground and space, are also presented: effective aperture diameter, depending on the degree of correction by adaptive optics (for 8 m Unit Telescopes (UTs) and 1.8 m Auxiliary Telescopes (ATs)); number of telescopes and (u, v) coverage possibilities; maximum size of the array (133/202 m with VIMA (VLTI Main Array)/VISA (VLTI Sub Array) respectively); wide field of view for off axis cophasing/coherencing (up to 8 arcsec field), thanks to the 'homothetic mapper'. In particular the size of the field of view has considerable impact on the scientific use of the VLTI and will be dealt with in more detail. After the year 2005, additional features may be available at the VLTI : four UTs and up to eight ATs and delay lines, with rapid reconfiguration of the array; partial adaptive optics at shorter wavelengths; blind operation by coherencing or cophasing from sources several arcmin away from axis; full sky coverage using laser guide stars for adaptive optics; cophasing of the array using in orbit artificial sources; and an extension of the VLTI towards the north of Paranal site. It is suggested that space programs in interferometry should complement large ground based facilities which will be operational by the first decade of the next century.

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