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Proceedings Paper

OHANA Phase III: scientific operation of an 800-meter Mauna Kea interferometer
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Paper Abstract

Once the proof of concept of the OHANA Array has been demonstrated, the Phase II capabilities can be put into regular science operation, and the OHANA facility can be upgraded to extend interferometric operation to include all of the telescopes of the OHANA Consortium member observatories. This will constitute the Phase III of OHANA. The technical developments required will be relatively straight-forward. Longer fiber sets will be procured (fiber losses are not a limiting factor at the OHANA scale). An enhanced delay line capability will be needed in order to exploit longer baselines with good sky coverage and ample super-synthesis (several compact, multi-pass long optical delay concepts are under investigation). The scheduling and operation modes of an instrument such as OHANA present interesting opportunities and complications. We envision a place for both collaborative consortium science, based on mutual allocation of facility access, and PI-driven access, based on telescope access exchange between consortium members. The most potentially successful mode of operation would imply a community driven model, open to proposals from the different time allocation comittees. This poster looks at possible methods of allocation and operation, inspired by the UKIRT infrared survey (UKIDSS), the European VLBI, and the very interesting possibility of a Mauna Kea telescope time exchange scheme. The issue of data property is of course intimately tied with the proposal/operation system, and means of data availability and distribution are discussed, along with data interpretation tools, which may be modeled on existing systems such as the ISC at Caltech or the JMMC in France. when weighed against the UV coverage, the potential science and the uniqueness of this project, all these issues are worth an in depth study. Discussions are starting as to an OHANA Operation Committee, the goal of which would be to discuss, define and eventually carry out operational modes. The goal, of course, is for the Operation Committee to handle the details of multi-telescope scheduling in a way that will be transparent to the scientist who merely seeks the observational results.

Paper Details

Date Published: 21 February 2003
PDF: 8 pages
Proc. SPIE 4838, Interferometry for Optical Astronomy II, (21 February 2003); doi: 10.1117/12.459740
Show Author Affiliations
Olivier Lai, Canada-France-Hawaii Telescope Corp. (United States)
Stephen T. Ridgway, Observatoire de Paris-Meudon (France)
National Optical Astronomy Observatories (United States)
Pierre J. Lena, Observatoire de Paris-Meudon (France)
Guy S. Perrin, Observatoire de Paris-Meudon (France)
Gregory Fahlman, Canada-France-Hawaii Telescope Corp. (United States)
Andrew J. Adamson, United Kingdom Infrared Telescope (United Kingdom)
Alan T. Tokunaga, Institute for Astronomy/Univ. of Hawaii (United States)
Jun Nishikawa, National Astronomical Observatory of Japan (United States)
Peter L. Wizinowich, W.M. Keck Observatory (United States)
Francois J. Rigaut, Gemini Observatory (United States)


Published in SPIE Proceedings Vol. 4838:
Interferometry for Optical Astronomy II
Wesley A. Traub, Editor(s)

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