First Results with the IOTA3 Imaging Interferometer: The Spectroscopic Binaries Virginis and WR 140

Monnier, John D.; Traub, W. A.; Schloerb, F. Peter; Millan-Gabet, R.; Berger, J.‐P.; Pedretti, E.; Carleton, N. P.; Kraus, Stefan; Lacasse, M. G.; Brewer, Michael K.; Ragland, Sam; Ahearn, A.; Coldwell, Charles M.; Haguenauer, Pierre; Kern, P.; Labeye, P.; Lagny, Laure; Malbet, Fabien; Malin, Daniella; Maymounkov, P.; Morel, S.; Papaliolios, C.; Perraut, K.; Pearlman, M. R.; Porro, I.; Schanen, Isabelle; Souccar, Kamal; Torres, Guillermo; Wallace, Gary

doi:10.1086/382213

Cited by 61 publications

(54 citation statements)

References 25 publications

(26 reference statements)

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“…Thus far, only two WR systems have been examined with interferometry. They are γ 2 Velorum (Hanbury Brown et al 1970, Millour et al 2007, North et al 2007) and WR 140 (Monnier et al 2004(Monnier et al , 2011. Both systems have well-defined doublelined spectroscopic orbits (Schmutz et al 1997, Fahed et al 2011) and consist of a carbon-rich WC star orbiting an O star.…”

Section: The Authorsmentioning

confidence: 99%

The CHARA Array resolves the long-period Wolf–Rayet binaries WR 137 and WR 138

Richardson

Shenar

Roy-Loubier

et al. 2016

Mon. Not. R. Astron. Soc.

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We report on interferometric observations with the CHARA Array of two classical Wolf-Rayet stars in suspected binary systems, namely WR 137 and WR 138. In both cases, we resolve the component stars to be separated by a few milliarcseconds. The data were collected in the H-band, and provide a measure of the fractional flux for both stars in each system. We find that the WR star is the dominant H-band light source in both systems ( f WR,137 = 0.59 ± 0.04; f WR,138 = 0.67 ± 0.01), which is confirmed through both comparisons with estimated fundamental parameters for WR stars and O dwarfs, as well as through spectral modeling of each system. Our spectral modeling also provides fundamental parameters for the stars and winds in these systems. The results on WR 138 provide evidence that it is a binary system which may have gone through a previous mass-transfer episode to create the WR star. The separation and position of the stars in the WR 137 system together with previous results from the IOTA interferometer provides evidence that the binary is seen nearly edge-on. The possible edge-on orbit of WR 137 aligns well with the dust production site imaged by the Hubble Space Telescope during a previous periastron passage, showing that the dust production may be concentrated in the orbital plane.

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Section: The Authorsmentioning

confidence: 99%

The CHARA Array resolves the long-period Wolf–Rayet binaries WR 137 and WR 138

Richardson

Shenar

Roy-Loubier

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We used the data reduction method described in Monnier et al (2004) to extract squared visibilities (V 2 ) and closure phases (CP) from the interferograms. Instrumental V 2 and CP effects were removed by interspersing each science target acquisition with observations of calibrators with small and known diameters.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

First astronomical unit scale image of the GW Orionis triple system

Berger

Monnier

Millan-Gabet

et al. 2011

A&A

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Context. Young and close multiple systems are unique laboratories to probe the initial dynamical interactions between forming stellar systems and their dust and gas environment. Their study is a key building block to understanding the high frequency of main-sequence multiple systems. However, the number of detected spectroscopic young multiple systems that allow dynamical studies is limited. GW Orionis is one such system. It is one of the brightest young T Tauri stars and is surrounded by a massive disk. Aims. Our goal is to probe the GW Orionis multiplicity at angular scales at which we can spatially resolve the orbit. Methods. We used the IOTA/IONIC3 interferometer to probe the environment of GW Orionis with an astronomical unit resolution in 2003, 2004, and 2005. By measuring squared visibilities and closure phases with a good UV coverage we carry out the first image reconstruction of GW Ori from infrared long-baseline interferometry. Results. We obtained the first infrared image of a T Tauri multiple system with astronomical unit resolution.We show that GW Orionis is a triple system, resolve for the first time the previously known inner pair (separation ρ ∼ 1.4 AU) and reveal a new more distant component (GW Ori C) with a projected separation of ∼8 AU with direct evidence of motion. Furthermore, the nearly equal (2:1) H-band flux ratio of the inner components suggests that either GW Ori B is undergoing a preferential accretion event that increases its disk luminosity or that the estimate of the masses has to be revisited in favour of a more equal mass-ratio system that is seen at lower inclination. Conclusions. Accretion disk models of GW Ori will need to be completely reconsidered because of this outer companion C and the unexpected brightness of companion B.

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“…The IO potential have been demontrated thanks to on-sky exploitation leading to astrophysical results using the IOTA interferometer (Mt Hopkins -Arizona ) [2,3] and the VLTI. Further in progress developments consider the use of complex IO components as VSI (VLTI Spectro Imager) [13] and Gravity [14] for the second generation instrument of the VLTI.…”

Section: Integrated Optics Applied To Interferometrymentioning

confidence: 99%

“…A limiting factor for the combination of all available beams of a given interferometer is this complexity and the induced high stability requirement. Using fiber optics and integrated optics devices one can address part of this concern [1] and efficient implementations on several instruments already provide noteworthy astrophysical results [2,3,4]. Major interferometric facilities, like the European Very Large Telescope Interferometer (VLTI -Cerro Paranal -Chile) (4x8 m telescopes and 4x1.8m telescopes) or Chara in Mt Wilson-California (6x1m telescopes) are currently operating instruments that make usage of photonics components and consider for their next generation instruments more complex photonics devices.…”

Section: Introductionmentioning

confidence: 99%

On-chip spectro-detection for fully integrated coherent beam combiners

Kern¹,

Coarer²,

Bénech³

2009

Opt. Express

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This paper presents how photonics associated with new arising detection technologies is able to provide fully integrated instrument for coherent beam combination applied to astrophysical interferometry. The feasibility and operation of on-chip coherent beam combiners has been already demonstrated using various interferometric combination schemes. More recently we proposed a new detection principle aimed at directly sampling and extracting the spectral information of an input signal together with its flux level measurement. The so-called SWIFTS demonstrated concept that stands for Stationary-Wave Integrated Fourier Transform Spectrometer, provides full spectral and spatial information recorded simultaneously thanks to a motionless detecting device. Due to some newly available detection principles considered for the implementation of the SWIFTS concept, some technologies can even provide photo-counting operation that brought a significant extension of the interferometry domain of investigation in astrophysics . The proposed concept is applicable to most of the interferometric instrumental modes including fringe tracking, fast and sensitive detection, Fourier spectral reconstruction and also to manage a large number of incoming beams. The paper presents three practical implementations, two dealing with pair-wise integrated optics beam combinations and the third one with an all-in-one 8 beam combination. In all cases the principles turned into a pair wise baseline coding after proper data processing.

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First Results with the IOTA3 Imaging Interferometer: The Spectroscopic Binaries Virginis and WR 140

Cited by 61 publications

References 25 publications

The CHARA Array resolves the long-period Wolf–Rayet binaries WR 137 and WR 138

The CHARA Array resolves the long-period Wolf–Rayet binaries WR 137 and WR 138

First astronomical unit scale image of the GW Orionis triple system

On-chip spectro-detection for fully integrated coherent beam combiners

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