Hostname: page-component-745bb68f8f-hvd4g Total loading time: 0 Render date: 2025-01-11T09:12:56.509Z Has data issue: false hasContentIssue false
  • English
  • Français

The VLT Interferometer

Published online by Cambridge University Press:  01 October 2007

A. Richichi
A. Richichi*
Affiliation:
European Southern Observatory, Karl-Schwarzschildstr. 2, 85748 Garching b. M., Germany email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The ESO Very Large Telescope Interferometer (VLTI) is arguably the most powerful optical interferometric facility available at present. In addition to the wide choice of baselines and the light collecting power of its 8.2 m and 1.8 m telescopes, the VLTI also offers a smooth and user-friendly operation which makes interferometry accessible to any astronomer and covers a wide range of scientific applications. Behind the routine scientific operations, however, the VLTI is in constant evolution. I will present some of the technological and instrumental improvements which are planned for the near and mid-term future, and discuss their implications for astrometry in particular. Among them, the PRIMA facility and the proposed GRAVITY instrument are designed to reach the level of 10 microarcseconds in the near-infrared.

Keywords

instrumentation: high angular resolutiontechniques: interferometricastrometry
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S248: A Giant Step: from Milli- to Micro-arcsecond Astrometry , October 2007 , pp. 44 - 47
Copyright
Copyright © International Astronomical Union 2008

References

Arsenault, R., Alonso, J., Bonnet, H. et al. 2003, in SPIE Proceedings, vol. 4839, p. 174Google Scholar
Bonaccini, D., Gallieni, D., Biasi, R. et al. 1997, in SPIE Proceedings, vol. 3126, p. 580Google Scholar
Glindemann, A., Algomedo, J., Amestica, R. et al. 2003, in SPIE Proceedings, vol. 4838, p. 89Google Scholar
Delplancke, F., Derie, F., Leveque, S. et al. 2006, in SPIE Proceedings, vol. 6268, p. 27Google Scholar
Gai, M., Menardi, S., Cesare, S. et al. 2004, in SPIE Proceedings, vol. 5491, p. 528Google Scholar
Gillessen, S., Perrin, G., Brandner, W. et al. 2006, in SPIE Proceedings, vol. 6268, p. 33Google Scholar
Gitton, P., Leveque, S., Avila, G., Phan Duc, T. 2004, in SPIE Proceedings, vol. 5491, p. 944Google Scholar
Hogenhuis, H., Visser, M., Derie, F. 2003, in SPIE Proceedings, vol. 4838, p. 1148Google Scholar
Kervella, P., Coude de Foresto, V., Glindemann, A. et al. 2000, in SPIE Proceedings, vol. 4006, p. 31Google Scholar
Leinert, C. 2004, in SPIE Proceedings, vol. 5491, p. 19Google Scholar
Morel, S., Vannier, M., Menardi, S. et al. 2004, in SPIE Proceedings, vol. 5491, p. 1079Google Scholar
Petrov, R., Malbet, F., Weigelt, G. et al. 2007 A&A, 464, 1Google Scholar