An integrated-optics 3-way beam combiner for IOTA

Berger, J.‐P.; Haguenauer, Pierre; Kern, P.; Rousselet-Perraut, K.; Malbet, Fabien; Gluck, Stéphane; Lagny, Laure; Schanen-Duport, Isabelle; Laurent, E.; Delboulbé, A.; Tatulli, E.; Traub, Wesley A.; Carleton, N. P.; Millan-Gabet, R.; Monnier, John D.; Pedretti, E.; Ragland, Sam

doi:10.1117/12.457983

Cited by 61 publications

(25 citation statements)

References 2 publications

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“…IOTA synthesized a total aperture size of 35 × 15 m, corresponding to an angular resolution of ≈10×23 milliarcsec at 1.65 μm. Squared visibility and closure phase (CP) measurements were obtained using the integrated optics combiner IONIC (Berger et al 2003). IOTA ceased operation in 2006 July.…”

Section: Observation and Data Reductionmentioning

confidence: 99%

The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

Lacour

Thiébaut

Perrin

et al. 2009

ApJ

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We present infrared interferometric imaging of the S-type Mira star χ Cygni. The object was observed at four different epochs in [2005][2006] with the Infrared-Optical Telescope Array optical interferometer (H band). Images show up to 40% variation in the stellar diameter, as well as significant changes in the limb darkening and stellar inhomogeneities. Model fitting gave precise time-dependent values of the stellar diameter, and reveals presence and displacement of a warm molecular layer. The star radius, corrected for limb darkening, has a mean value of 12.1 mas and shows a 5.1 mas amplitude pulsation. Minimum diameter was observed at phase 0.94 ± 0.01. Maximum temperature was observed several days later at phase 1.02 ± 0.02. We also show that combining the angular acceleration of the molecular layer with CO (Δv = 3) radial velocity measurements yields a 5.9 ± 1.5 mas parallax. The constant acceleration of the CO molecules-during 80% of the pulsation cycle-lead us to argument for a free-falling layer. The acceleration is compatible with a gravitational field produced by a 2.1 +1.5 −0.7 solar mass star. This last value is in agreement with fundamental mode pulsator models. We foresee increased development of techniques consisting in combining radial velocity with interferometric angular measurements, ultimately allowing total mapping of the speed, density, and position of the diverse species in pulsation-driven atmospheres.

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Section: Observation and Data Reductionmentioning

confidence: 99%

The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

Lacour

Thiébaut

Perrin

et al. 2009

ApJ

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“…This combination optical circuit allows a pairwise beam combination between the three beams (Berger et al 2003). Two of the optical paths are scanned with piezo translation stages (see telescope section).There are therefore 6 interferometric outputs and no photometric channel since real-time photometry can be estimated from interferometric signals.…”

Section: The Beam Combinermentioning

confidence: 99%

A laboratory interferometer simulator for integrated optics combiners qualification

Jocou

Benisty

Berger

et al. 2004

New Frontiers in Stellar Interferometry

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We present a laboratory interferometer simulator specifically designed to characterize prototype integrated optics combiners. In the current configuration it allows to simulate a complex object made of luminous points and observe it with a reconfigurable array made of three telescopes. We used a three-way integrated optics similar to the one used at IOTA to combine the beams. We describe it in detail and present first validation measurements and first measurements of a binary star. This work paves the way for an up-to eight telescope simulator capable of simulating the VLTI and the VITRUV focal instrument.

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“…The data presented in this paper were obtained using the near-IR IONIC3 beam combiner. 3 The beam combiner produces two complementary outputs for each of the three interferometer baselines. These outputs are detected by IOTA's PICNIC-camera.…”

Section: Observationsmentioning

confidence: 99%

Infrared imaging of Capella with the IOTA interferometer

Kraus

Schloerb

2004

New Frontiers in Stellar Interferometry

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We present near infrared aperture synthesis maps of the well known binary star Capella (α Aur) produced with the upgraded IOTA interferometer on top of Mount Hopkins, Arizona. Michelson interferograms were obtained simultaneously on three interferometer baselines in the H-band between 2002 November 12 and 16. The simultaneous observation of fringes on three baselines permitted a single phase closure to be estimated along with three visibility amplitudes. Hybrid Mapping techniques were then used to reconstruct the source brightness distribution with a beam size of (5.4 × 2.6) mas, which allows for the resolution of the stellar surfaces of the Capella giants. The maps provide the first demonstration of imaging with phase closure on the IOTA instrument.

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An integrated-optics 3-way beam combiner for IOTA

Abstract: We report the here the first visibility and closure-phase measurements done with the IONIC instrument at the IOTA interferometer. The IONIC instrument is presented and preliminary analysis of the results discussed. Future improvements of IONIC are envisioned.

Cited by 61 publications

References 2 publications

The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

A laboratory interferometer simulator for integrated optics combiners qualification

Infrared imaging of Capella with the IOTA interferometer

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