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Eclipsing binaries are instrumental to our understanding of fundamentalstellar parameters. With the arrival of ultra-wide cameras and large areaphotometric monitoring programs, numerous eclipsing binaries systems have beenreported photometrically. However, due to the expensive efforts to follow upthem spectroscopically, most of their basic properties remain unexplored. Inthis paper we exploited the eclipsing binary light curves delivered by theall-sky Catalina sky surveys, in tandem with the single shot spectroscopicsurvey from SDSS, and identify a double-lined M-dwarf eclipsing binarySDSSJ1156-0207. Because this system is very faint (V=15.89 mag), we obtainedfollow-up radial velocity measurements using Gemini Multi-Object Spectrographonboard Gemini north telescope. This provides us a spectral resolution R~4000,enabling us to determine the mass and radius of each stellar components whenjointly fitted with light curve. Our best-fit results indicate that bothcomponents are of M dwarf, with the primary component to be 0.54+/-0.20 M_sunand 0.46+/-0.08 R_sun, while the secondary component to be 0.19+/-0.08 M_sunand 0.30+/-0.08 R_sun. High resolution spectroscopic observations in the futurewill help pin down the stellar parameters, providing insights to the stellarmodels at low mass regimes, as well as shedding lights on the internalstructure of close-in low mass objects and their inflation mechanism.

SDSSJ1156-0207: A 0.54 M_sun + 0.19 M_sun Double-lined M Dwarf Eclipsing Binary System