TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Abstract

Context. Multiple stellar systems play a fundamental role in the formation and evolution of stellar populations in galaxies. Recent and ongoing large ground-based multi-object spectroscopic surveys significantly increase the sample of spectroscopic binaries (SBs) allowing analyses of their statistical properties. Aims. We investigate the repeated spectral observations of the Gaia-ESO Survey internal data release 5 (GES iDR5) to identify and characterise SBs with one visible component (SB1s) in fields covering mainly the discs, the bulge, the CoRot fields, and some stellar clusters and associations. Methods. A statistical χ 2 -test is performed on spectra of the iDR5 subsample of approximately 43 500 stars characterised by at least two observations and a signal-to-noise ratio larger than three. In the GES iDR5, most stars have four observations generally split into two epochs. A careful estimation of the radial velocity (RV) uncertainties is performed. Our sample of RV variables is cleaned from contamination by pulsation-and/or convection-induced variables using Gaia DR2 parallaxes and photometry. Monte-Carlo simulations using the SB9 catalogue of spectroscopic orbits allow to estimate our detection efficiency and to correct the SB1 rate to evaluate the GES SB1 binary fraction and its relation to effective temperature and metallicity. Results. We find 641 (resp., 803) FGK SB1 candidates at the 5σ (resp., 3σ) level. The maximum RV differences range from 2.2 km s −1 at the 5σ confidence level (1.6 km s −1 at 3σ) to 133 km s −1 (in both cases). Among them a quarter of the primaries are giant stars and can be located as far as 10 kpc. The orbital-period distribution is estimated from the RV standard-deviation distribution and reveals that the detected SB1s probe binaries with log P[d] 4. We show that SB1s with dwarf primaries tend to have shorter orbital periods than SB1s with giant primaries. This is consistent with binary interactions removing shorter period systems as the primary ascends the red giant branch. For two systems, tentative orbital solutions with periods of 4 and 6 d are provided. After correcting for detection efficiency, selection biases, and the present-day mass function, we estimate the global GES SB1 fraction to be in the range 7-14% with a typical uncertainty of 4%. A small increase of the SB1 frequency is observed from K-towards F-type stars, in agreement with previous studies. The GES SB1 frequency decreases with metallicity at a rate of (−9 ± 3)% dex −1 in the metallicity range −2.7 ≤[Fe/H]≤ +0.6. This anticorrelation is obtained with a confidence level higher than 93% on a homogeneous sample covering spectral types FGK and a large range of metallicities. When the present-day mass function is accounted for, this rate turns to (−4 ± 2)% dex −1 with a confidence level higher than 88%. In addition we provide the variation of the SB1 fraction with metallicity separately for F, G, and K spectral types, as well as for dwarf and giant primaries.

The GALAH survey: multiple stars and our Galaxy

“…We applied conservative selection criteria to obtain our final sample of binary stars, but the true number of binaries in the data is much greater. Our detection methods might be further improved in order to extend the sample towards longer orbital periods and lower mass ratios (see also the methods in El-Badry et al 2018 andMerle et al 2020).…”

The Gaia-ESO Survey: Spectroscopic-asteroseismic analysis of K2 stars in Gaia-ESO

“…Gaia-ESO, on the other hand, determines RVs for every star, regardless of their binary status. Indeed, a special working group within Gaia-ESO (WG14) analyses double-line spectroscopic binaries and peculiar stars, flagging every target prior to the spectral analysis (Merle et al 2017(Merle et al , 2020. None of the stars in this sample have been flagged as a double-line spectroscopic binary or as a peculiar star by WG14.…”

Double-lined spectroscopic binaries in the APOGEE DR16 and DR17 data

“…To build a sizable sample of candidates that can be used for rigorous statistics, it is necessary to obtain spectra of > 10 5 −10 6 sources, ideally over the course of several epochs. Studies of this nature are becoming increasingly common with large spectroscopic surveys, such as RAVE (e.g., Matijevič et al 2010;Birko et al 2019), LAMOST (e.g., Tian et al 2020), Gaia-ESO (e.g., Merle et al 2017Merle et al , 2020, GALAH (e.g., Traven et al 2020), and SDSS APOGEE (e.g., Fernandez et al 2017;Skinner et al 2018;.…”