| Issue |
A&A
Volume 672, April 2023
|
|
|---|---|---|
| Article Number | A119 | |
| Number of page(s) | 30 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202245712 | |
| Published online | 10 April 2023 | |
The Araucaria project: High-precision orbital parallaxes and masses of binary stars
I. VLTI/GRAVITY observations of ten double-lined spectroscopic binaries⋆
1
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile
e-mail: alexandre.gallenne@gmail.com
2
French-Chilean Laboratory for Astronomy, IRL 3386, CNRS, Casilla 36-D, Santiago, Chile
3
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
4
LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris-Diderot, 5 place Jules Janssen, 92195 Meudon, France
5
Centrum Astronomiczne im. Mikołaja Kopernika, Polish Academy of Sciences, Rabiańska 8, 87-100 Toruń, Poland
6
Centrum Astronomiczne im. Mikołaja Kopernika, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland
Received:
17
December
2022
Accepted:
8
February
2023
Aims. We aim to measure very precise and accurate model-independent masses and distances of detached binary stars. Precise masses at the < 1% level are necessary to test and calibrate stellar interior and evolution models, while precise and independent orbital parallaxes are essential to check for the next Gaia data releases.
Methods. We combined RV measurements with interferometric observations to determine orbital and physical parameters of ten double-lined spectroscopic systems. We report new relative astrometry from VLTI/GRAVITY and, for some systems, new VLT/UVES spectra to determine the radial velocities of each component.
Results. We measured the distance of ten binary systems and the mass of their components with a precision as high as 0.03% (average level 0.2%). They are combined with other stellar parameters (effective temperatures, radii, flux ratios, etc.) to fit stellar isochrones and determine their evolution stage and age. We also compared our orbital parallaxes with Gaia and showed that half of the stars are beyond 1σ with our orbital parallaxes; although, their RUWE is below the frequently used cutoff of 1.4 for reliable Gaia astrometry. By fitting the telluric features in the GRAVITY spectra, we also estimated the accuracy of the wavelength calibration to be ∼0.02% in high and medium spectral resolution modes.
Conclusions. We demonstrate that combining spectroscopic and interferometric observations of binary stars provides extremely precise and accurate dynamical masses and orbital parallaxes. As they are detached binaries, they can be used as benchmark stars to calibrate stellar evolution models and test the Gaia parallaxes.
Key words: binaries: general / binaries: spectroscopic / techniques: high angular resolution / astrometry / binaries: close / techniques: radial velocities
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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