Creevey, O. L.Benedict, G. F.Brown, T. M.Alonso, R.Cargile, P.Mandushev, G.Charbonneau, D.McArthur, B. E.Cochran, W.O'Donovan, F. T.Jiménez-Reyes, S. J.Belmonte, J. A.Kolinski, D.2019-09-272005Creevey, O. L., G. F. Benedict, T. M. Brown, R. Alonso, P. Cargile, G. Mandushev, D. Charbonneau, et al. 2005. “A New Detached M Dwarf Eclipsing Binary.” The Astrophysical Journal 625 (2): L127–30. https://doi.org/10.1086/431278.2041-82052041-8213http://nrs.harvard.edu/urn-3:HUL.InstRepos:41417372We describe a newly discovered detached M dwarf eclipsing binary system. This system was first observed by the TrES network during a long-term photometry campaign of 54 nights. Analysis of the folded light curve indicates two very similar components orbiting each other with a period of 1.12079 +/- 0.00001 days. Spectroscopic observations with the Hobby-Eberly Telescope show the system to consist of two M3e dwarfs in a near-circular orbit. Double-line radial velocity amplitudes, combined with the orbital inclination derived from light-curve fitting, yield M-total = 0.983 +/- 0.007 M-circle dot with component masses of M-1 = 0.493 +/- 0.003 M-circle dot and M-2 = The light-curve fit yields component radii of R-1 = 0.489 +/- 0.003 R-circle dot and R-2 = 0.452 +/- 0.050 R-circle dot. Although a precise parallax is lacking, broadband VJHK colors and spectral typing suggest component 0.050 absolute magnitudes of and. M (1) = 11.18 +/- 0.30 M (2) = 11.28 +/- 0.30.en-USJournal Article2019-09-2710.1086/431278