Volume 606, October 2017
|Number of page(s)||7|
|Published online||29 September 2017|
Image of the close companion in front of the primary
1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
2 Dpt. Astronomia i Astrofísica, Universitat de València, C/Dr. Moliner 50, 46100 Burjassot, Spain
3 Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía S/N, 18008 Granada, Spain
4 Centro Astronómico Hispano Alemán, Calar Alto, (CSIC-MPG), Sierra de los Filabres, 04550 Gergal, Spain
5 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Lagrange, CS 34229, 06304 Nice Cedex 4, France
6 Observatori Astronòmic, Universidad de València, 46980 Paterna, Spain
7 European Southern Observatory, Casilla 19001, Santiago 19, Chile
8 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
9 South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa
10 Astronomy Department, University of Cape Town, 7701 Rondebosch, South Africa
11 National Institute for Theoretical Physics, Private Bag X1, 7602 Matieland, South Africa
12 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
Received: 14 July 2017
Accepted: 4 September 2017
Context. The star V766 Cen (=HR 5171A) was originally classified as a yellow hypergiant but lately found to more likely be a 27−36 M⊙ red supergiant (RSG). Recent observations indicated a close eclipsing companion in the contact or common-envelope phase.
Aims. Here, we aim at imaging observations of V766 Cen to confirm the presence of the close companion.
Methods. We used near-infrared H-band aperture synthesis imaging at three epochs in 2014, 2016, and 2017, employing the PIONIER instrument at the Very Large Telescope Interferometer (VLTI).
Results. The visibility data indicate a mean Rosseland angular diameter of 4.1 ± 0.8 mas, corresponding to a radius of 1575 ± 400 R⊙. The data show an extended shell (MOLsphere) of about 2.5 times the Rosseland diameter, which contributes about 30% of the H-band flux. The reconstructed images at the 2014 epoch show a complex elongated structure within the photospheric disk with a contrast of about 10%. The second and third epochs show qualitatively and quantitatively different structures with a single very bright and narrow feature and high contrasts of 20−30%. This feature is located toward the south-western limb of the photospheric stellar disk. We estimate an angular size of the feature of 1.7 ± 0.3 mas, corresponding to a radius of 650 ± 150 R⊙, and giving a radius ratio of 0.42+0.35-0.10 compared to the primary stellar disk.
Conclusions. We interpret the images at the 2016 and 2017 epochs as showing the close companion, or a common envelope toward the companion, in front of the primary. At the 2014 epoch, the close companion is behind the primary and not visible. Instead, the structure and contrast at the 2014 epoch are typical of a single RSG harboring giant photospheric convection cells. The companion is most likely a cool giant or supergiant star with a mass of 5+15-3 M⊙.
Key words: techniques: interferometric / stars: massive / stars: imaging / supergiants / binaries: eclipsing / binaries: close
Based on observations made with the VLT Interferometer at Paranal Observatory under programme IDs 092.D-0096, 092.C-0312, and 097.D-0286.
© ESO, 2017
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