Nathan De Lee, Jian Ge, Justin R. Crepp, Jason Eastman, Massimiliano Esposito, Bruno Femenía, Scott W. Fleming, B. Scott Gaudi, Luan Ghezzi, Jonay I. González Hernández, Brian L. Lee, Keivan G. Stassun, John P. Wisniewski, W. Michael Wood-Vasey, Eric Agol, Carlos Allende Prieto, Rory Barnes, Dmitry Bizyaev, Phillip Cargile, Liang Chang, Luiz N. Da Costa, G. F. Porto De Mello, Leticia D. Ferreira, Bruce Gary, Leslie Hebb, Jon Holtzman, Jian Liu, Bo Ma, Claude E. Mack III, Suvrath Mahadevan, Marcio A. G. Maia, Duy Cuong Nguyen, Audrey Oravetz, Daniel J. Oravetz, Martin Paegert, Kaike Pan, Joshua Pepper, Elena Malanushenko, Viktor Malanushenko, Rafael Rebolo, Basilio X. Santiago, Donald P. Schneider, Alaina C. Shelden Bradley, Xiaoke Wan, Ji Wang, Bo Zhao
We describe the discovery of a likely brown dwarf (BD) companion with a minimum mass of 31.7 +/- 2.0 M_Jup to GSC 03546-01452 from the MARVELS radial velocity survey, which we designate as MARVELS-6b. For reasonable priors, our analysis gives a probability of 72% that MARVELS-6b has a mass below the hydrogen-burning limit of 0.072 M_Sun, and thus it is a high-confidence BD companion. It has a moderately long orbital period of 47.8929 +0.0063/-0.0062 days with a low eccentricty of 0.1442 +0.0078/-0.0073, and a semi-amplitude of 1644 +12/-13 m/s. Moderate resolution spectroscopy of the host star has determined the following parameters: T_eff = 5598 +/- 63, log g = 4.44 +/- 0.17, and [Fe/H] = +0.40 +/- 0.09. Based upon these measurements, GSC 03546-01452 has a probable mass and radius of M_star = 1.11 +/- 0.11 M_Sun and R_star = 1.06 +/- 0.23 R_Sun with an age consistent with less than ~6 Gyr at a distance of 219 +/- 21 pc from the Sun. Although MARVELS-6b is not observed to transit, we cannot definitively rule out a transiting configuration based on our observations. There is a visual companion detected with Lucky Imaging at 7.7 arcsec from the host star, but our analysis shows that it is not bound to this system. The minimum mass of MARVELS-6b exists at the minimum of the mass functions for both stars and planets, making this a rare object even compared to other BDs.
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http://arxiv.org/abs/1304.2815
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