2007/07/31 by Cullen H. Blake, Guillermo Torres, Joshua S. Bloom +2
Mathematics · Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Low Mass #Mathematics #Photometry (optics) #Physics #Sky #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/589630
published as Astrophys.J.684:635-643,2008 · 15 Pages, 9 Figures, 6 Tables. Replaced with version accepted to ApJ
arxiv created 2008/06/17 · openalex publication_date 2008/08/26 · arxiv updated 2010/04/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present observations of a new low-mass, double-lined eclipsing binary system discovered using repeat observations of the celestial equator from the Sloan Digital Sky Survey II. Using near-infrared photometry and optical spectroscopy we have measured the properties of this short-period [ P = 0.407037(14) days] system and its two components. We find the following parameters for the two components: M 1 = 0.272 ± 0.020 M ☉ , R 1 = 0.268 ± 0.010 R ☉ , M 2 = 0.240 ± 0.022 M ☉ , R 2 = 0.248 ± 0.0090 R ☉ , T 1 = 3320 ± 130 K, and T 2 = 3300 ± 130 K. The masses and radii of the two components of this system agree well with theoretical expectations based on models of low-mass stars, within the admittedly large errors. Future synoptic surveys like Pan-STARRS and LSST will produce a wealth of information about low-mass eclipsing systems and should make it possible, with an increased reliance on follow-up observations, to detect many systems with low-mass and substellar companions. With the large numbers of objects for which these surveys will produce high-quality photometry, we suggest that it becomes possible to identify such systems even with sparse time sampling and a relatively small number of individual observations.