2018AJ....155...86L

Eclipsing binaries are instrumental to our understanding of fundamental stellar parameters. With the arrival of ultra-wide cameras and large area photometric monitoring programs, numerous eclipsing binaries systems have been reported photometrically. However, due to the expensive efforts to follow up spectroscopically, most of their basic properties remain unexplored. In this paper, we exploited the eclipsing binary light curves delivered by the all-sky catalina sky surveys, in tandem with the single shot spectroscopic survey from SDSS, and identify a double-lined M-dwarf eclipsing binary SDSSJ1156-0207. Because this system is very faint (V = 15.89 mag), we obtained follow-up radial velocity measurements using the Gemini Multi-object Spectrograph on board the Gemini North Telescope. This provides us with a spectral resolution R ∼ 4000, enabling us to determine the mass and radius of each of the stellar components when jointly fitted with light curve. Our best-fit results indicate that both components are from the M dwarf, with the primary component being 0.54±0.20 M_☉ and 0.46±0.08 R_☉, while the secondary component is 0.19±0.08 M_☉ and 0.30±0.08 R_☉. High-resolution spectroscopic observations in the future will help pin down the stellar parameters, providing insights into the stellar models at low-mass regimes, as well as sheding light on the internal structure of close-in low-mass objects and their inflation mechanism.