The VLT Interferometer-Reference-Cited by-同舟云学术

The VLT Interferometer

Published:1994 Issue: Volume:158 Page:143-150
ISSN:0074-1809
Container-title:Symposium - International Astronomical Union
language:en
Short-container-title:Symp. - Int. Astron. Union

Author:

Bedding T. R.,Beckers J. M.,Faucherre M.,Hubin N.,Koehler B.,von der Lühe O.,Merkle F.,Zhu N.

Abstract

One of the observing modes available with the ESO Very Large Telescope will be coherent combination of the light received by up to four 8 m unit telescopes and several 1.8 m auxiliary telescopes. The location of the main telescopes is fixed, while auxiliary telescopes can be moved among some 30 observing stations. The locations of these stations were chosen to augment the (u, v) coverage of the unit telescopes as well as to function as an independent interferometric array.The 8 m telescopes will be equipped with adaptive optics to correct for seeing-induced wavefront aberrations. This wavefront correction will be complete at near-infrared wavelengths, giving the interferometer very high sensitivity in this spectral regime. This paper gives a brief description of the VLT Interferometer and an update on its status.

Publisher

Cambridge University Press (CUP)

Reference12 articles.

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2. von der Lühe O. , Beckers J. M. , and Braun R. , 1992b, The configuration of the VLT Interferometer on the Paranal site, in Proceedings of the ESO Conference on High-Resolution Imaging by Interferometry II, edited by Beckers J. M. and Merkle F. , p. 959, Garching bei München, F.R.G., October 1991.

3. Plathner D. and Beckers J. M. , 1992, The design of the Auxiliary Telescopes for the VLT Interferometer, in Proceedings of the ESO Conference on High-Resolution Imaging by Interferometry II, edited by Beckers J. M. and Merkle F. , p. 939, Garching bei München, F.R.G., October 1991.

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