Infrared Imaging of Capella with the IOTA Closure Phase Interferometer

Kraus, Stefan; Schloerb, F. Peter; Traub, W. A.; Carleton, N. P.; Lacasse, M. G.; Pearlman, M. R.; Monnier, John D.; Millan-Gabet, R.; Berger, J.‐P.; Haguenauer, Pierre; Perraut, K.; Kern, P.; Malbet, Fabien; Labeye, P.

doi:10.1086/430456

Cited by 27 publications

(31 citation statements)

References 20 publications

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“…To account for time smearing across the observing blocks, we computed the triple model at 10 second intervals and averaged over the complex visibilities. We also accounted for bandwidth smearing which reduces the fringe coherence at separations comparable to the width of the fringe packet following the formalism in Kraus et al (2005). Summing the visibilities at the location of each component, the complex visibility of a triple system is given by,…”

Section: Chara Astrometric Resultsmentioning

confidence: 99%

Orbits, Distance, and Stellar Masses of the Massive Triple Star Σ Orionis

Schaefer¹,

Hummel²,

Gies³

et al. 2016

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We present interferometric observations of the σ Orionis triple system using the CHARA Array, NPOI, and VLTI. Using these measurements, we spatially resolve the orbit of the close spectroscopic binary (Aa,Ab) for the first time and present a revised orbit for the wide pair (A,B). Combining the visual orbits with previously published radial velocity measurements and new radial velocities measured at CTIO, we derive dynamical masses for the three massive stars in the system of M Aa = 16.99 ± 0.20 M ⊙ , M Ab = 12.81 ± 0.18 M ⊙ , and M B = 11.5 ± 1.2 M ⊙ . The inner and outer orbits in the triple are not coplanar, with a relative inclination of 120• -127• . The orbital parallax provides a precise distance of 387.5 ± 1.3 pc to the system. This is a significant improvement over previous estimates of the distance to the young σ Orionis cluster.

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Section: Chara Astrometric Resultsmentioning

confidence: 99%

Orbits, Distance, and Stellar Masses of the Massive Triple Star Σ Orionis

Schaefer¹,

Hummel²,

Gies³

et al. 2016

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“…The closure phase, unaffected by atmopheric effects, is a prerequisite for determining asymmetries in the measured brightness distribution, so essential for image reconstruction (e.g., Jennison 1958; Leinert 1992). However, numerous interferometric observations are necessary for an acceptable image (Kraus et al 2005). Therefore, the closure phase is not discussed any further in this study.…”

Section: Observations With Iotamentioning

confidence: 99%

Multiwavelength interferometric observations and modeling of circumstellar disks

Schegerer

Ratzka

Schuller

et al. 2013

A&A

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Aims. We investigate the structure of the innermost region of three circumstellar disks around pre-main sequence stars HD 142666, AS 205 N, and AS 205 S. We determine the inner radii of the dust disks and, in particular, search for transition objects where dust has been depleted and inner disk gaps have formed at radii of a few tenths of AU up to several AU. Methods. We performed interferometric observations with IOTA, AMBER, and MIDI in the infrared wavelength ranges 1.6−2.5 μm and 8−13 μm with projected baseline lengths between 25 m and 102 m. The data analysis was based on radiative transfer simulations in 3D models of young stellar objects (YSOs) to reproduce the spectral energy distribution and the interferometric visibilities simultaneously. Accretion effects and disk gaps could be considered in the modeling approach. Results from previous studies restricted the parameter space. Results. The objects of this study were spatially resolved in the infrared wavelength range using the interferometers. Based on these observations, a disk gap could be found for the source HD 142666 that classifies it as transition object. There is a disk hole up to a radius of R in = 0.30 AU and a (dust-free) ring between 0.35 AU and 0.80 AU in the disk of HD 142666. The classification of AS 205 as a system of classical T Tauri stars could be confirmed using the canonical model approach, i.e., there are no hints of disk gaps in our observations.

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“…A similar approach is applied to the model visibilities V model (λ) (which we compute using Eqs. (7), (11), and (12) from Kraus et al 2005):…”

Section: Modelingmentioning

confidence: 99%

“…The measured closure phases are fit simultaneously with the differential visibilities, weighting each data point according to the determined error bars (see Eqs. (8)- (10) in Kraus et al 2005). Parameters in our binary star model are the binary separation ρ, the position angle Θ, the intensity ratio F C2 /F C1 , and the uniform disk diameter of the components.…”

Section: Modelingmentioning

confidence: 99%

“…2.2), we did not use the H-band data for image reconstruction and rejected also one measurement taken under particularly poor and variable conditions (2007 Dec. 05, UT 07:46). In order to correct for the binary orbital motion over the 3-month period (Δρ = 2.2 mas, ΔΘ = 6.6 • ), we apply a rotation-compensating coordinate transformation of the uv-plane (see Kraus et al 2005, for a description of this procedure) using the astrometric data given in Table 3. Then, we employed our Building Block Mapping software, which is based on the algorithm described by Hofmann & Weigelt (1993).…”

Section: Vlti/amber Aperture Synthesis Imagingmentioning

confidence: 99%

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Tracing the young massive high-eccentricity binary system $\theta^{\mathsf 1}$Orionis C through periastron passage

Kraus¹,

Weigelt²,

Balega

et al. 2009

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106

102

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Context. The nearby high-mass star binary system θ 1 Ori C is the brightest and most massive of the Trapezium OB stars at the core of the Orion Nebula Cluster, and it represents a perfect laboratory to determine the fundamental parameters of young hot stars and to constrain the distance of the Orion Trapezium Cluster. Aims. By tracing the orbital motion of the θ 1 Ori C components, we aim to refine the dynamical orbit of this important binary system. Methods. Between January 2007 and March 2008, we observed θ 1 Ori C with VLTI/AMBER near-infrared (H-and K-band) longbaseline interferometry, as well as with bispectrum speckle interferometry with the ESO 3.6 m and the BTA 6 m telescopes (Band V -band). Combining AMBER data taken with three different 3-telescope array configurations, we reconstructed the first VLTI/AMBER closure-phase aperture synthesis image, showing the θ 1 Ori C system with a resolution of ∼2 mas. To extract the astrometric data from our spectrally dispersed AMBER data, we employed a new algorithm, which fits the wavelength-differential visibility and closure phase modulations along the H-and K-band and is insensitive to calibration errors induced, for instance, by changing atmospheric conditions. Results. Our new astrometric measurements show that the companion has nearly completed one orbital revolution since its discovery in 1997. The derived orbital elements imply a short-period (P ≈ 11.3 yr) and high-eccentricity orbit (e ≈ 0.6) with periastron passage around 2002.6. The new orbit is consistent with recently published radial velocity measurements, from which we can also derive the first direct constraints on the mass ratio of the binary components. We employ various methods to derive the system mass (M system = 44 ± 7 M ) and the dynamical distance (d = 410 ± 20 pc), which is in remarkably good agreement with recently published trigonometric parallax measurements obtained with radio interferometry.

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Infrared Imaging of Capella with the IOTA Closure Phase Interferometer

Cited by 27 publications

References 20 publications

Orbits, Distance, and Stellar Masses of the Massive Triple Star Σ Orionis

Orbits, Distance, and Stellar Masses of the Massive Triple Star Σ Orionis

Multiwavelength interferometric observations and modeling of circumstellar disks

Tracing the young massive high-eccentricity binary system $\theta^{\mathsf 1}$Orionis C through periastron passage

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