Gaia Data Release 3: spectroscopic binary-star orbital solutions and the SB1 processing chain
Creators
- 1. Institut d'Astrophysique et de Géophysique, Université de Liège, 19c, Allée du 6 Août, B-4000 Liège, Belgium
- 2. CRAAG-Centre de Recherche en Astronomie, Astrophysique et Géophysique, Route de l'Observatoire, Bp 63 Bouzareah, DZ- 16340 Algiers, Algeria
- 3. Université de Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550, 11 rue de l'Université, F-67000 Strasbourg, France
- 4. Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles CP 226, Boulevard du Triomphe, B-1050 Brussels, Belgium
- 5. INAF - Osservatorio Astrofisico di Torino, via Osservatorio 20, I-10025 Pino Torinese (TO), Italy
- 6. GEPI, Observatoire de Paris, Université PSL, CNRS, 5 Place Jules Janssen, F-92190 Meudon, France
Description
Context. The Gaia satellite constitutes one of the cornerstone missions of ESA. This is an astrometric space experiment that is measuring positions, proper motions as well as parallaxes for a huge number of stars. It is also performing photometric and spectrophotometric observations. Gaia also operates a medium-dispersion spectrometer, the RVS, that provides spectra and thus radial velocity (RV) time-series.
Aims. The paper is centred on the analysis of the RV time-series. We try to fit orbital models and trend models and restrict ourselves to the objects of spectral types F-G-K brighter than magnitude 12 presenting only one single spectrum (SB1).
Methods. Suitable time-series are processed and analysed object per object, providing orbital or trend solutions. The results of the various fits are further filtered internally on the basis of several quality measures in order to discard spurious solutions. The objects only having a spectroscopic solution are classified in one of the three classes SB1 (eccentric model), SB1C (circular model) or TrendSB1 (mere trend model).
Results. We detail the methods used and describe the derived parameters and results. After a description of the models considered, and of the related quality tests of the fit, we detail the internal filtering that is intended to reject bad solutions. We also present a full validation of the pipeline. A description of the current content of the catalogue is provided. We present the SB1, SB1C and the TrendSB1 spectroscopic solutions contained in the SB-subcatalogue which is part of the DR3 catalogue. 
Conclusions. We delivered some 181327 orbital solutions in the class SB1, 202 in the class SB1C and 56808 in the associated class TrendSB1. This is a first release and the delivered SB-subcatalogue could be tuned and refined. However the majority of the entries are correct; this data set constitutes by far the largest set of spectroscopic orbital solutions ever constituted.
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Additional details
Dates
- Accepted
- 
      2024-10-08