'OHANA phase II: a prototype demonstrator of fiber-linked interferometry between very large telescopes

Perrin, G.; Lai, Olivier; Woillez, J.; Guerin, Jean; Reynaud, François; Ridgway, Stephen T.; Léna, Pierre; Wizinowich, Peter; Tokunaga, A. T.; Nishikawa, Jun; Rigaut, François; Adamson, A. J.; Guyon, Olivier

doi:10.1117/12.459382

Cited by 10 publications

(4 citation statements)

References 7 publications

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“…We expect to start a part of the scientific observing runs in the fall of 2004 for stars selected suitably for our interferometer, single stars, binaries, and variables. Large array proposals as `OHANA 10,11,12,13,14 and the next stage of MIRA 10,15 are also in sight for us. The latter consists of D>1m, B>500m, and N>3 telescopes, and we hope to make further considerations how to realize it.…”

Section: Discussionmentioning

confidence: 99%

MIRA-I.2: recent progress

Nishikawa

Yoshizawa

Ohishi

et al. 2004

New Frontiers in Stellar Interferometry

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After the first fringe detection with MIRA-I.2 30m baseline for Vega in June 2002, fringes for Vega and Deneb has been confirmed and then construction continued. Fast delay line has been evacuated and extended from 4m to 8m long. Coarse delay line has been extended from 2m to 4m. Baseline vector has been determined with 0.1mm accuracy. Aluminized mirrors have been changed to gold-plated ones, and the total throughput has become four times larger than before at the 600nm-1000nm band. The photon rate is 150 per ms for a 2 mag (I-band) star and the present limiting magnitude is better than 3mag. A delay modulation PZT has been set to push a cat's eye retro-reflector. Observations have been made for 6 stars with successful fringe packet detections. Visibility stability has been being studied with artificial light sources and Vega, which preliminary results are better than a few percent. A three-color system between 600-1000nm is now on the half way of installation. Gregorian cat's eye retro-reflectors with fine delay line PZTs and fringe tracking control software is planned to be installed.

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Section: Discussionmentioning

confidence: 99%

MIRA-I.2: recent progress

Nishikawa

Yoshizawa

Ohishi

et al. 2004

New Frontiers in Stellar Interferometry

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“…The use of single mode fibers for beam transport might be crucial for the heterodyne architecture. Much work has been done in this area for the OHANA 21 project and new lab results were recently presented at this meeting (Anderson et al).…”

Section: Technology Spotlightsmentioning

confidence: 99%

Planet formation imager (PFI): introduction and technical considerations

et al. 2014

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Complex non-linear and dynamic processes lie at the heart of the planet formation process. Through numerical simulation and basic observational constraints, the basics of planet formation are now coming into focus. High resolution imaging at a range of wavelengths will give us a glimpse into the past of our own solar system and enable a robust theoretical framework for predicting planetary system architectures around a range of stars surrounded by disks with a diversity of initial conditions. Only long-baseline interferometry can provide the needed angular resolution and wavelength coverage to reach these goals and from here we launch our planning efforts. The aim of the "Planet Formation Imager" (PFI) project is to develop the roadmap for the construction of a new near-/mid-infrared interferometric facility that will be optimized to unmask all the major stages of planet formation, from initial dust coagulation, gap formation, evolution of transition disks, mass accretion onto planetary embryos, and eventual disk dispersal. PFI will be able to detect the emission of the cooling, newlyformed planets themselves over the first 100 Myrs, opening up both spectral investigations and also providing a vibrant look into the early dynamical histories of planetary architectures.Here we introduce the Planet Formation Imager (PFI) Project (www.planetformationimager.org) and give initial thoughts on possible facility architectures and technical advances that will be needed to meet the challenging top-level science requirements.

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“…OHANA 13 has the maximum baseline of 800m which requires a compensation of a few hundred meters delay under no exclusive delay line building condition. In the Phase II of the project, a delay line system of +-40m for the early stages is considered to be put in the coude room of CFHT 14 , because Keck delay line system will not be always available for various baselines of OHANA. It is desirable to construct a delay line system for hundreds of meters delay in the CFHT room for the late stages 15,16 .…”

Section: An 800m Delay Line Concept For Ohana At Cfhtmentioning

confidence: 99%

Long-baseline optical fiber interferometer instruments and science

et al. 2003

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b MIRA project, National Astronomical Observatory of Japan Developments of fiber linked optical interferometer are reported. This interferometer is a part of MIRA-I.2 interferometer (Mitaka InfraRed and optical Array). MIRA-I.2 is an optical interferometer with a 30 meters long baseline. It consists of two 30cm siderostats, tip-tilt mirrors, vacuum pipes delay lines and detectors. We plan to use two 60 meters long polarization-maintaining fibers for arms of the interferometer, instead of vacuum pipes. The developments include dispersion and polarization compensation of fiber and fiber injection module. In laboratory experiments, dispersion compensation succeeded. The fringe visibility was 0.93 for wide-band, where the central wavelength of light was 700nm, and bandwidth was 200nm, while 0.95 with a He-Ne laser. We used BK7 glass wedge for dispersion compensation. About fiber injection module, basic optical design has completed. The results of our fiber interferometer could contribute to OHANA (Optical Hawaiian Array for Nanoradian Astronomy) project. We present new science targets, white dwarves and T Tauri stars, and an 800m delayline concept in CFHT for the project.

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'OHANA phase II: a prototype demonstrator of fiber-linked interferometry between very large telescopes

Cited by 10 publications

References 7 publications

MIRA-I.2: recent progress

MIRA-I.2: recent progress

Planet formation imager (PFI): introduction and technical considerations

Long-baseline optical fiber interferometer instruments and science

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