arXiv:1403.1583v1 [astro-ph.SR] 6 Mar 2014 The Catalogue of Stellar Parameters from the Detached Double-Lined Eclipsing Binaries in the Milky Way Z. Eker A,* , S. Bilir B , F. Soydugan C,D , E. Yaz G¨ ok¸ ce B , E. Soydugan C,D , M. T¨ uys¨ uz C,D , T. S ¸eny¨ uz C,D , O. Demircan D,E A Akdeniz University, Faculty of Sciences, Department of Space Sciences and Technologies, 07058, Antalya, Turkey B Istanbul University, Faculty of Sciences, Department of Astronomy and Space Sciences, 34119, University-Istanbul, Turkey C C ¸anakkale Onsekiz Mart University, Faculty of Sciences and Arts, Department of Physics, 17100 C ¸anakkale, Turkey D C ¸anakkale Onsekiz Mart University, Astrophysics Research Center and Ulupınar Observatory, 17100 C ¸ anakkale, Turkey E C ¸anakkale Onsekiz Mart University, Faculty of Sciences and Arts, Department of Space Science and Technologies, 17020 C ¸anakkale, Turkey ∗ Email: eker@akdeniz.edu.tr Abstract: The most accurate stellar astrophysical parameters were collected from the solutions of the light and the radial velocity curves of 257 detached double-lined eclipsing binaries in the Milky Way. The catalogue contains masses, radii, surface gravities, effective temperatures, luminosities, projected rotational velocities of the component stars and the orbital parameters. The number of stars with accurate parameters increased 67 per cent in comparison to the most recent similar collection by Torres et al. (2010). Distributions of some basic parameters were investigated. The ranges of effective temperatures, masses and radii are 2750 <T ef f (K)< 43000, 0.18 < M/M⊙ < 33 and 0.2 < R/R⊙ < 21.2, respectively. Being mostly located in one kpc in the Solar neighborhood, the present sample covers distances up to 4.6 kpc within the two local Galactic arms Carina-Sagittarius and Orion Spur. The number of stars with both mass and radius measurements better than 1 per cent uncertainty is 93, better than 3 per cent uncertainty is 311, and better than 5 per cent uncertainty is 388. It is estimated from the Roche lobe filling factors that 455 stars (88.5 per cent of the sample) are spherical within 1 per cent of uncertainty. Keywords: Stars: fundamental parameters – Stars: binaries: eclipsing – Stars: binaries: spectroscopic – Astronomical Data based: catalogues 1 Introduction Nearly sixty percent or more of the Solar neighborhood stars are binaries or multiple systems (Duquennoy & Mayor 1993). Bi- naries are important for astrophysicists not only because they over populate single stars, but also because they provide basic stellar parameters as independent observed quantities used in testing astrophysical theories. Stellar masses can be determined directly via application of Kepler’s law for the visual binaries if apparent orbital parameters were calibrated to be real. A cal- ibration is possible for a visual pair if its distance (parallax) is known. Reliable stellar masses could also be obtained from the radial velocity curves without distance, but only if orbital incli- nations were known. The resolved double stars (visual binaries confirmed to be spectroscopic binaries), therefore, are a special case to provide reliable stellar masses, since the orbital inclina- tions are from the apparent orbit and the absolute orbital sizes are from the radial velocity curves. Gainfully, the light curves of eclipsing binaries could pro- vide orbital inclinations and the radii relative to the semi-major axis of the orbit. But, if both stars are resolved spectroscopi- cally, accurately determined radii and masses could be obtained from the simultaneous solutions of the light and the radial ve- locity curves. In addition to the radii, which are not available from visual binaries, the eclipsing spectroscopic binaries provide masses, effective temperatures and the absolute dimensions of the orbit, from which absolute brightnesss could be calculated. Provided with a parallax, either the physical parameters or the parallax could mutually be tested by comparing the photomet- ric and the trigonometric distance moduli. Otherwise, a proper solution would provide not only the most reliable stellar param- eters, but also a reliable photometric distance (parallax) as an independent quantity. The critical compilations of stellar parameters and absolute dimensions of binary components were initiated, and continued with increasing quantity and quality especially by Popper (1980) and Harmanec (1988). Andersen (1991) collected accurate stel- lar masses and radii with uncertainties less than 2 per cent from the detached, double-lined eclipsing systems. The list contained 45 (90 stars) binaries which are all non-interacting, so that each star could be accepted as if evolved as single stars. Accuracies of 1-2 per cent were found to be significant for deeper astrophys- ical insight than merely improving the spectrum of masses and radii. Due to great sensitivity of other parameters, only limited amount of useful results could be extracted up to ±5 per cent uncertainties. Malkov (1993) announced a catalog of astrophysical param- eters of binary systems containing 114 systems including all pre and out of main sequence, contact and semi-contact systems. Gorda & Svechnikov (1998) collected stellar masses and radii with accuracies better than 2-3 per cent from photometric, ge- ometric, and absolute elements of 112 eclipsing binaries with 1