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• W4288083105 endingPage "A145" @default.
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• W4288083105 abstract "Context. Binary stellar systems form a large fraction of the Galaxy’s stars. They are useful as laboratories for studying the physical processes taking place within stars, and must be correctly taken into account when observations of stars are used to study the structure and evolution of the Galaxy. The advent of large-scale spectroscopic and photometric surveys allows us to obtain large samples of binaries that permit characterising their populations. Aims. We aim to obtain a large sample of double-lined spectroscopic binaries (SB2s) by analysis of spectra from the GALAH survey in combination with photometric and astrometric data. A combined analysis will provide stellar parameters of thousands of binary stars that can be combined to form statistical observables of a given population. We aim to produce a catalogue of well-characterised systems, which can in turn be compared to models of populations of binary stars, or to follow-up individual systems of interest. Methods. We obtained a list of candidate SB2 systems from a t-distributed stochastic neighbour embedding (t-SNE) classification and a cross-correlation analysis of GALAH spectra. To compute parameters of the primary and secondary star, we used a Bayesian approach that includes a parallax prior from Gaia DR2, spectra from GALAH, and apparent magnitudes from APASS, Gaia DR2, 2MASS, and WISE. We used a Markov chain Monte Carlo approach to sample the posterior distributions of the following model parameters for the two stars: T eff[1,2] , log g [1,2] , [Fe/H], V r [1,2] , v mic[1,2] , v broad[1,2] , R [1,2] , and E ( B − V ). Results. We present results for 12 760 binary stars detected as SB2s. We construct the statistical observables T 1 ∕ T 2 , Δ V r , and R 1 ∕ R 2 , which demonstrate that our sample mostly consists of dwarfs, with a significant fraction of evolved stars and several dozen members of the giant branch. The majority of these binary stars is concentrated at the lower boundary of the Δ V r distribution, and the R 1 ∕ R 2 ratio is mostly close to unity. The derived metallicity of our binary stars is statistically lower than that of single dwarf stars from the same magnitude-limited sample. Conclusions. Our sample of binary stars represents a large population of well-characterised double-lined spectroscopic binaries that are appropriate for statistical studies of the binary populations. The derived stellar properties and their distributions show trends that are expected for a population of close binary stars ( a < 10 AU) detected through double lines in their spectra. Our detection technique allows us to probe binary systems with mass ratios 0.5 ≤ q ≤ 1." @default.
• W4288083105 created "2022-07-28" @default.
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• W4288083105 date "2020-06-01" @default.
• W4288083105 modified "2023-10-15" @default.
• W4288083105 title "The GALAH survey: multiple stars and our Galaxy" @default.
• W4288083105 cites W1490864757 @default.
• W4288083105 cites W1836177459 @default.
• W4288083105 cites W1851037028 @default.
• W4288083105 cites W1963642624 @default.
• W4288083105 cites W2000054184 @default.
• W4288083105 cites W2003246319 @default.
• W4288083105 cites W2003427934 @default.
• W4288083105 cites W2005436942 @default.
• W4288083105 cites W2017020311 @default.
• W4288083105 cites W2052937506 @default.
• W4288083105 cites W2096433368 @default.
• W4288083105 cites W2104168804 @default.
• W4288083105 cites W2109138120 @default.
• W4288083105 cites W2111817932 @default.
• W4288083105 cites W2126597027 @default.
• W4288083105 cites W2142220522 @default.
• W4288083105 cites W2148977774 @default.
• W4288083105 cites W2153495170 @default.
• W4288083105 cites W2167635287 @default.
• W4288083105 cites W2237029308 @default.
• W4288083105 cites W2342657640 @default.
• W4288083105 cites W2415887386 @default.
• W4288083105 cites W2474034009 @default.
• W4288083105 cites W2509043249 @default.
• W4288083105 cites W2567715800 @default.
• W4288083105 cites W2577537660 @default.
• W4288083105 cites W2593224863 @default.
• W4288083105 cites W2737701238 @default.
• W4288083105 cites W2751237541 @default.
• W4288083105 cites W2755365622 @default.
• W4288083105 cites W2761986865 @default.
• W4288083105 cites W2769510393 @default.
• W4288083105 cites W2776003291 @default.
• W4288083105 cites W2781957983 @default.
• W4288083105 cites W2784067869 @default.
• W4288083105 cites W2796946405 @default.
• W4288083105 cites W2797738305 @default.
• W4288083105 cites W2798158223 @default.
• W4288083105 cites W2798336535 @default.
• W4288083105 cites W2798436812 @default.
• W4288083105 cites W2804103092 @default.
• W4288083105 cites W2885087496 @default.
• W4288083105 cites W2895216826 @default.
• W4288083105 cites W2909432773 @default.
• W4288083105 cites W2936494458 @default.
• W4288083105 cites W2949380767 @default.
• W4288083105 cites W2977390572 @default.
• W4288083105 cites W2978552137 @default.
• W4288083105 cites W2982528647 @default.
• W4288083105 cites W2991076082 @default.
• W4288083105 cites W3011221771 @default.
• W4288083105 cites W3037126510 @default.
• W4288083105 cites W3098483445 @default.
• W4288083105 cites W3098601396 @default.
• W4288083105 cites W3099330186 @default.
• W4288083105 cites W3099528176 @default.
• W4288083105 cites W3099619931 @default.
• W4288083105 cites W3099886124 @default.
• W4288083105 cites W3100900517 @default.
• W4288083105 cites W3100934019 @default.
• W4288083105 cites W3101482359 @default.
• W4288083105 cites W3101779292 @default.
• W4288083105 cites W3102014803 @default.
• W4288083105 cites W3102098446 @default.
• W4288083105 cites W3102386126 @default.
• W4288083105 cites W3103411869 @default.

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