OHANA

Guy Perrin; Olivier Lai; Julien Woillez; Jean Guerin; Takayuki Kotani; Sébastien Vergnole; Andy J. Adamson; Christ Ftaclas; Olivier Guyon; Pierre Léna; Jun Nishikawa; François Reynaud; Kathy Roth; Stephen T. Ridgway; Alan T. Tokunaga; Peter L. Wizinowich

doi:10.1117/12.551585

OHANA

Guy Perrin, Olivier Lai, Julien Woillez, Jean Guerin, Takayuki Kotani, Sébastien Vergnole, Andy J. Adamson, Christ Ftaclas, Olivier Guyon, Pierre Léna, Jun Nishikawa, François Reynaud, Kathy Roth, Stephen T. Ridgway, Alan T. Tokunaga, Peter L. Wizinowich

Research output: Contribution to journal › Conference article › peer-review

8 Scopus citations

Abstract

The Mauna Kea Observatory offers a unique opportunity to build a large and sensitive interferometer. Seven telescopes have diameters larger than 3 meters and are or may be equipped with adaptive optics systems to correct phase perturbations induced by atmospheric turbulence. The maximum telescope separation of 800 meters can provide an angular resolution as good as 0.25 milli-arcseconds in the J band. The large pupils and long baselines make 'OHANA very complementary to existing large optical interferometers. From an astrophysical point of view, it opens the way to imaging of the central part of faint and compact objects such as active galactic nuclei and young stellar objects. On a technical point of view, it opens the way to kilometric or more arrays by propagating light in single-mode fibers. First instruments have been built and tested successfully at CFHT, Keck I and Gemini to inject light into single-mode fibers thus partly completing Phase I of the project. Phase II is now on-going with the prospects of the first combinations of Keck I - Keck II in 2004 and Gemini - CFHT in 2005.

Original language	English (US)
Article number	43
Pages (from-to)	391-404
Number of pages	14
Journal	Proceedings of SPIE - The International Society for Optical Engineering
Volume	5491
Issue number	PART 1
DOIs	https://doi.org/10.1117/12.551585
State	Published - 2004
Externally published	Yes
Event	New Frontiers in Stellar Interferometry - Glasgow, United Kingdom Duration: Jun 21 2004 → Jun 25 2004

Keywords

Adaptive Optics
Interferometry
OHANA
Single-mode fiber

ASJC Scopus subject areas

Electronic, Optical and Magnetic Materials
Condensed Matter Physics
Computer Science Applications
Applied Mathematics
Electrical and Electronic Engineering

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10.1117/12.551585

Cite this

Perrin, G., Lai, O., Woillez, J., Guerin, J., Kotani, T., Vergnole, S., Adamson, A. J., Ftaclas, C., Guyon, O., Léna, P., Nishikawa, J., Reynaud, F., Roth, K., Ridgway, S. T., Tokunaga, A. T., & Wizinowich, P. L. (2004). OHANA. Proceedings of SPIE - The International Society for Optical Engineering, 5491(PART 1), 391-404. Article 43. https://doi.org/10.1117/12.551585

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abstract = "The Mauna Kea Observatory offers a unique opportunity to build a large and sensitive interferometer. Seven telescopes have diameters larger than 3 meters and are or may be equipped with adaptive optics systems to correct phase perturbations induced by atmospheric turbulence. The maximum telescope separation of 800 meters can provide an angular resolution as good as 0.25 milli-arcseconds in the J band. The large pupils and long baselines make 'OHANA very complementary to existing large optical interferometers. From an astrophysical point of view, it opens the way to imaging of the central part of faint and compact objects such as active galactic nuclei and young stellar objects. On a technical point of view, it opens the way to kilometric or more arrays by propagating light in single-mode fibers. First instruments have been built and tested successfully at CFHT, Keck I and Gemini to inject light into single-mode fibers thus partly completing Phase I of the project. Phase II is now on-going with the prospects of the first combinations of Keck I - Keck II in 2004 and Gemini - CFHT in 2005.",

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author = "Guy Perrin and Olivier Lai and Julien Woillez and Jean Guerin and Takayuki Kotani and S{\'e}bastien Vergnole and Adamson, {Andy J.} and Christ Ftaclas and Olivier Guyon and Pierre L{\'e}na and Jun Nishikawa and Fran{\c c}ois Reynaud and Kathy Roth and Ridgway, {Stephen T.} and Tokunaga, {Alan T.} and Wizinowich, {Peter L.}",

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doi = "10.1117/12.551585",

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note = "New Frontiers in Stellar Interferometry ; Conference date: 21-06-2004 Through 25-06-2004",

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AU - Perrin, Guy

AU - Lai, Olivier

AU - Woillez, Julien

AU - Guerin, Jean

AU - Kotani, Takayuki

AU - Vergnole, Sébastien

AU - Adamson, Andy J.

AU - Ftaclas, Christ

AU - Guyon, Olivier

AU - Léna, Pierre

AU - Nishikawa, Jun

AU - Reynaud, François

AU - Roth, Kathy

AU - Ridgway, Stephen T.

AU - Tokunaga, Alan T.

AU - Wizinowich, Peter L.

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N2 - The Mauna Kea Observatory offers a unique opportunity to build a large and sensitive interferometer. Seven telescopes have diameters larger than 3 meters and are or may be equipped with adaptive optics systems to correct phase perturbations induced by atmospheric turbulence. The maximum telescope separation of 800 meters can provide an angular resolution as good as 0.25 milli-arcseconds in the J band. The large pupils and long baselines make 'OHANA very complementary to existing large optical interferometers. From an astrophysical point of view, it opens the way to imaging of the central part of faint and compact objects such as active galactic nuclei and young stellar objects. On a technical point of view, it opens the way to kilometric or more arrays by propagating light in single-mode fibers. First instruments have been built and tested successfully at CFHT, Keck I and Gemini to inject light into single-mode fibers thus partly completing Phase I of the project. Phase II is now on-going with the prospects of the first combinations of Keck I - Keck II in 2004 and Gemini - CFHT in 2005.

AB - The Mauna Kea Observatory offers a unique opportunity to build a large and sensitive interferometer. Seven telescopes have diameters larger than 3 meters and are or may be equipped with adaptive optics systems to correct phase perturbations induced by atmospheric turbulence. The maximum telescope separation of 800 meters can provide an angular resolution as good as 0.25 milli-arcseconds in the J band. The large pupils and long baselines make 'OHANA very complementary to existing large optical interferometers. From an astrophysical point of view, it opens the way to imaging of the central part of faint and compact objects such as active galactic nuclei and young stellar objects. On a technical point of view, it opens the way to kilometric or more arrays by propagating light in single-mode fibers. First instruments have been built and tested successfully at CFHT, Keck I and Gemini to inject light into single-mode fibers thus partly completing Phase I of the project. Phase II is now on-going with the prospects of the first combinations of Keck I - Keck II in 2004 and Gemini - CFHT in 2005.

KW - Adaptive Optics

KW - Interferometry

KW - OHANA

KW - Single-mode fiber

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OHANA

Abstract

Keywords

ASJC Scopus subject areas

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