scholarly journals ESO 16 Metre Very Large Telescope: The Linear Array Concept

1984 ◽  
Vol 79 ◽  
pp. 767-787
Author(s):  
Daniel Enard
Keyword(s):  
Adaptive Optics ◽  
Linear Array ◽  
Cost Effective ◽  
Visible Range ◽  
Large Telescope ◽  
New Developments ◽  
Very Large Telescope ◽  
Coherent Coupling ◽  
Set Up ◽  
Large Telescopes

VLT preliminary studies were initiated at ESO as early as 1978 (1). After ESO's move from Geneva to Munich (1980) a study group chaired first by R. Wilson, then by J.P. Swings was set up and among a number of conceptual ideas that were analysed, the concept of a “limited array” emerged as the most attractive (2). A significant driver was then, interferometry; however after a theoretical analysis performed by F. Roddier and P. Lena (3), it became clear that interferometry with large telescopes would not be cost-effective in the visible range. In the IR, the situation would be more favorable but the overall efficiency would depend on factors that are not reliably known at present. The conclusion was that it might be difficult to justify a huge investment too exclusively oriented towards interferometry, such as an array of movable large telescopes, but on the other hand the possibility of a coherent coupling in the IR should be maintained as a prime requirement since new developments in detectors and in adaptive optics could make it effective and scientifically very rewarding.

scholarly journals NAOMI: the adaptive optics system of the Auxiliary Telescopes of the VLTI

2019 ◽  
Vol 629 ◽  
pp. A41 ◽  
Author(s):  
J. Woillez ◽  
J. A. Abad ◽  
R. Abuter ◽  
E. Aller Carpentier ◽  
J. Alonso ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Single Mode ◽  
Large Telescope ◽  
Wavefront Correction ◽  
Design Performance ◽  
Very Large Telescope ◽  
Fringe Tracking ◽  
Adaptive Optics System ◽  
Atmospheric Seeing

Context. The tip-tilt stabilisation system of the 1.8 m Auxiliary Telescopes of the Very Large Telescope Interferometer was never dimensioned for robust fringe tracking, except when atmospheric seeing conditions are excellent. Aims. Increasing the level of wavefront correction at the telescopes is expected to improve the coupling into the single-mode fibres of the instruments, and enable robust fringe tracking even in degraded conditions. Methods. We deployed a new adaptive optics module for interferometry (NAOMI) on the Auxiliary Telescopes. Results. We present its design, performance, and effect on the observations that are carried out with the interferometric instruments.

scholarly journals Summary – A Personal View

1998 ◽  
Vol 11 (2) ◽  
pp. 689-691
Author(s):  
Kazimierz StȩpieŃ
Keyword(s):  
Large Telescope ◽  
Personal View ◽  
Very Large Telescope ◽  
The Subject ◽  
The Right ◽  
Large Telescopes

Let me first remind you of the subject of the present Joint Discussion. It is about spectroscopy with large telescopes. As I have never done any spectroscopic research of my own and I have never observed with a very large telescope, I am certainly the right person to summarize the most recent results in this area.

scholarly journals A FOSSIL BULGE GLOBULAR CLUSTER REVEALED BY VERY LARGE TELESCOPE MULTI-CONJUGATE ADAPTIVE OPTICS

2011 ◽  
Vol 737 (1) ◽  
pp. 31 ◽  
Author(s):  
Sergio Ortolani ◽  
Beatriz Barbuy ◽  
Yazan Momany ◽  
Ivo Saviane ◽  
Eduardo Bica ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Globular Cluster ◽  
Large Telescope ◽  
Very Large Telescope

scholarly journals Replicated spectrographs in astronomy

2014 ◽  
Vol 3 (3) ◽  
Author(s):  
Gary J. Hill
Keyword(s):  
Adaptive Optics ◽  
Large Scale ◽  
Mechanical Stability ◽  
Cost Effective ◽  
Lessons Learned ◽  
Full Potential ◽  
Astronomical Instruments ◽  
Very Large Telescope ◽  
Small Fields ◽  
Future Technologies

AbstractAs telescope apertures increase, the challenge of scaling spectrographic astronomical instruments becomes acute. The next generation of extremely large telescopes (ELTs) strain the availability of glass blanks for optics and engineering to provide sufficient mechanical stability. While breaking the relationship between telescope diameter and instrument pupil size by adaptive optics is a clear path for small fields of view, survey instruments exploiting multiplex advantages will be pressed to find cost-effective solutions. In this review we argue that exploiting the full potential of ELTs will require the barrier of the cost and engineering difficulty of monolithic instruments to be broken by the use of large-scale replication of spectrographs. The first steps in this direction have already been taken with the soon to be commissioned MUSE and VIRUS instruments for the Very Large Telescope and the Hobby-Eberly Telescope, respectively. MUSE employs 24 spectrograph channels, while VIRUS has 150 channels. We compare the information gathering power of these replicated instruments with the present state of the art in more traditional spectrographs, and with instruments under development for ELTs. Design principles for replication are explored along with lessons learned, and we look forward to future technologies that could make massively-replicated instruments even more compelling.

scholarly journals Interstellar Matter with Very Large Telescopes

1984 ◽  
Vol 79 ◽  
pp. 675-678
Author(s):  
J. Lequeux
Keyword(s):  
High Resolution ◽  
Absorption Lines ◽  
High Resolution Spectroscopy ◽  
Interstellar Matter ◽  
Large Telescope ◽  
Interstellar Absorption ◽  
Near Ir ◽  
Very Large Telescope ◽  
Large Telescopes ◽  
Diffuse Matter

Interstellar matter is certainly one of the fields where a very large telescope (VLT) will prove to be most fruitful. This includes (somewhat paradoxically, but this will be explained later) the study of extended emissions. I will now examine in turn the different domains of interest for a VLT.I. Neutral diffuse matterOptical and near IR observations will mainly contribute to this domain through high-resolution spectroscopy of interstellar absorption lines in the spectra of stars. These lines are resonant lines of atoms (NaI, KI, etc.) or ions (CaII, TiII, etc.) as well as of some molecules (CH+, CH, CN, CS+, C2 in the near IR). Clearly this kind of study is always photon - limited; a VLT will collect more photons than present telescopes, thus increase the possibilities considerably.

scholarly journals Extremely Large Telescopes on the Antarctic plateau

2005 ◽  
Vol 13 ◽  
pp. 956-957
Author(s):  
J.S. Lawrence
Keyword(s):  
Adaptive Optics ◽  
Turbulence Structure ◽  
Large Telescope ◽  
Dome A ◽  
Antarctic Plateau ◽  
Guide Star ◽  
Laser Guide ◽  
Large Telescopes ◽  
The Antarctic ◽  
Adaptive Optics System

AbstractThe primary limitation to the performance of any large ground-based telescope is the atmospheric properties of its site, particularly the sky emission and the turbulence structure. There are several sites on the Antarctic plateau (South Pole, Dome C and Dome A) for which the increase in infrared sensitivity relative to a mid-latitude site should be as much as two orders of magnitude. The unique turbulent structure above Dome C indicates that an extremely large telescope equipped with only a natural guide star adaptive optics system should achieve equivalent resolution to a mid-latitude extremely large telescope with a multi-conjugate multi-laser guide star system.

Adaptive optics system for the Very Large Telescope

1994 ◽  
Author(s):  
Norbert N. Hubin ◽  
Bertrand Theodore ◽  
Patrick Petitjean ◽  
Bernard Delabre
Keyword(s):  
Adaptive Optics ◽  
Large Telescope ◽  
Very Large Telescope ◽  
Adaptive Optics System

scholarly journals Uses of Very Large Telescopes for Galaxy Research

1984 ◽  
Vol 79 ◽  
pp. 703-711 ◽  
Author(s):  
M.-H. Ulrich
Keyword(s):  
Elliptical Galaxies ◽  
Point Sources ◽  
High Spectral Resolution ◽  
Large Field ◽  
Large Telescope ◽  
Quasar Spectra ◽  
Very Large Telescope ◽  
Large Telescopes ◽  
Field Imaging

SummaryMany areas of extragalactic research will greatly benefit from observations with a very large telescope. We concentrate, here, on four of them as illustrative examples:First we briefly discuss the study of the absorption lines in quasar spectra.In the second section we suggest the possibility of doing serendipity large field imaging during high spectral resolution exposures on point sources.In sections 3 and 4 we discuss two topics which have long been recognized as important drivers for the construction of very large telescopes, the determination of the nature of the missing mass, and the study of elliptical galaxies.

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