Volume 601, May 2017
|Number of page(s)||21|
|Section||Stellar structure and evolution|
|Published online||25 April 2017|
1 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
2 Institute of Astrophysics, KU Leuven, Celestijnlaan 200D, 3001 Leuven, Belgium
3 Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, 19C Allée du Six Août, 4000 Liège, Belgium
4 European Southern Observatory, Schwarzschild-Str. 2, 85748 Garching bei München, Germany
5 Unidad Mixta Internacional Franco-Chilena de Astronomía (UMI 3386), CNRS/INSU France; Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
6 LESIA, UMR 8109, Observatoire de Paris, CNRS, UPMC, Univ. Paris-Diderot, PSL, 5 place Jules Janssen, 92195 Meudon, France
7 European Southern Observatory, Alonso de Cordova 3107, Vitacura, 19001 Casilla, Santiago 19, Chile
8 I. physikalisches Institut, Universität zu Köln, Zülpicherstr. 77, 50937 Köln, Germany
9 Instituto de Astrofisica, Facultad de Fisica, Pontificia Universidad Católica de Chile, Casilla 306, 22 Santiago, Chile
10 University of Exeter, Astrophysics Group, School of Physics, Stocker Road, Exeter EX4 4QL, UK
11 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
Received: 7 July 2016
Accepted: 23 July 2016
Aims. Our long-term aim is to derive model-independent stellar masses and distances for long period massive binaries by combining apparent astrometric orbit with double-lined radial velocity amplitudes (SB2).
Methods. We followed-up ten O+O binaries with AMBER, PIONIER and GRAVITY at the VLTI. Here, we report on 130 astrometric observations over the last seven years. We combined this dataset with distance estimates to compute the total mass of the systems. We also computed preliminary individual component masses for the five systems with available SB2 radial velocities.
Results. Nine of the ten binaries have their three-dimensional orbit well constrained. Four of them are known to be colliding wind, non-thermal radio emitters, and thus constitute valuable targets for future high angular resolution radio imaging. Two binaries break the correlation between period and eccentricity tentatively observed in previous studies. This suggests either that massive star formation produces a wide range of systems, or that several binary formation mechanisms are at play. Finally, we found that the use of existing SB2 radial velocity amplitudes can lead to unrealistic masses and distances.
Conclusions. If not understood, the biases in radial velocity amplitudes will represent an intrinsic limitation for estimating dynamical masses from SB2+interferometry or SB2+Gaia. Nevertheless, our results can be combined with future Gaia astrometry to measure the dynamical masses and distances of the individual components with an accuracy of 5 to 15%, completely independently of the radial velocities.
Key words: stars: massive / binaries: general / methods: observational / techniques: high angular resolution
Based on observations collected with the PIONIER/VLTI, AMBER/VLTI and GRAVITY/VLTI instruments at the European Southern Observatory, Paranal, under programs 087.C-0458, 087.D-0150, 087.D-0264, 090.D-0036, 090.D-0291, 090.D-0600, 091.D-0087, 091.D-0334, 092.C-0243, 092.C-0542, 092.D-0015, 092.D-0366, 092.D-0590, 092.D-0647, 093.C-0503, 093.D-0039, 093.D-0040, 093.D-0673, 094.C-0397, 094.C-0884, 189.C-0644, 60.A-9168, 096.D-0114.
The list of astrometric positions is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/601/A34
© ESO, 2017
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.