NASA ADS Astronomy Abstract Service

Title:
OHANA phase II: a prototype demonstrator of fiber linked interferometry between very large telescopes
Authors:
Perrin, Guy S.; Lai, Olivier; Woillez, Julien; Guerin, Jean; Reynaud, Francois; Ridgway, Stephen T.; Lena, Pierre J.; Wizinowich, Peter L.; Tokunaga, Alan T.; Nishikawa, Jun; Rigaut, Francois J.; Adamson, Andrew J.; Guyon, Olivier
Affiliation:
AA(Observatoire de Paris-Meudon (France)), AB(Canada-France-Hawaii Telescope Corp. (USA)), AC(Observatoire de Paris-Meudon (France)), AD(Observatoire de Paris-Meudon (France)), AE(Univ. de Limoges (France)), AF(National Optical Astronomy Observatory (USA)), AG(Observatoire de Paris-Meudon (France)), AH(W.M. Keck Observatory (USA)), AI(Institute for Astronomy/Univ. of Hawaii (USA)), AJ(National Astronomical Observatory of Japan (USA)), AK(Gemini Observatory (USA)), AL(United Kingdom Infrared Telescope (United Kingdom)), AM(Institute for Astronomy/Univ. of Hawaii (USA))
Journal:
Interferometry for Optical Astronomy II. Edited by Wesley A. Traub . Proceedings of the SPIE, Volume 4838, pp. 1290-1295 (2003). (SPIE Homepage)
Publication Date:
02/2003
Origin:
SPIE
Abstract Copyright:
(c) 2003: SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Bibliographic Code:
2003SPIE.4838.1290P

Abstract

The ‘OHANA (Optical Hawaiian Array for Nanoradian Astronomy, means "family" in Hawaiian) aims at making a large and sensitive optical/IR array with the Mauna Kea 3 to 10 meter telescopes. Telescopes will be linked with single-mode fibers to carry the coherence of the beams from the output of the telescopes adaptive optics systems to the beam combination units. The project has been divided into three phases. The first phase is dedicated to the injection of light into single-mode fibers and to the building of the injection module. The third phase is the realization of the complete array and its use by a wide community of astronomers. In the second phase, a prototype ‘OHANA will be built and the "shortest" baselines will be explored. The baselines will be located in the South-East and West parts of the observatory. An extra baseline will possibly link the two groups of telescopes if infrastructure comply with it. This phase II ‘OHANA will already be the longest and most sensitive optical/IR interferometer built. Scientific targets will span young stellar objects, extragalactic sources and other types of astronomical topics which require both high angular resolution and sensitivity. This paper reviews the main characteristics of the phase II interferometer.