Publications of the MPIfR
Optical & Infrared
Interferometry Group
D. Mourard, P.Antonelli, A. Blazit, D.
Bonneau, Y. Bresson, J.M.Clausse, A. Domiciano, M. Dugué, R. Foy, P.
Harmanec, M. Heininger, K.H. Hofmann, S. Jankov,
P. Koubsky, S. Lagarde, J.B.Lebouquin, P. Mathias, A. Meilland, N.
Nardetto, R. Petrov, K. Rousselet-Perraut, D. Schertl, Ph. Stee, I.
Tallon-Bosc, M. Tallon, E. Thiébaut, F. Vakili, G. Weigelt
VEGA: a visible spectrograph and polarimeter
for the VLTI (invited paper)
"ESO Astrophysics Symposia"
Proceedings of the ESO Workshop: "The power of
optical/IR interferometry: recent scientific results and 2nd generation
VLTI instrumentation"
April 4-8, 2005 in Garching, Germany
pg.395-406 (2008)
Abstract
The ESO/VLTI has now clearly a position of world leader in the do-
main of ground based optical interferometry. With 4 telescopes of 8m20
and 2 (4)
telescopes of 1m80, the Paranal Observatory is without any doubt the
best optical
interferometric facility in the world. Since many years, it has
concentrated the ma-
jor part of the European interferometric community and with the opening
of MIDI
and AMBER, the astronomers have now access to 'general user'
interferometric
instruments in the thermal and near infrared. This paper describes a
project for a
second generation focal instrument of the VLTI, named VEGA for Visible
spEc-
troGraph and polArimeter. The goal is to give access to the visible
wavelengths,
with spectroscopic and polarimetric capabilities and taking advantage
of the coher-
ent field of view of the VLTI. It is a new unique scientific niche for
the VLTI, in
the international competition. For example, a 200m interferometer
operating in the
visible will be able to resolve structures of the order of 0.1 AU at
the distance of
the Ophucius cloud.
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