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25 April 2024

» arxiv » 1202.4964

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Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars from MARVELS I: A Low Mass Ratio Stellar Companion to TYC 4110-01037-1 in a 79-day Orbit
John P. Wisniewski ; Jian Ge ; Justin R. Crepp ; Nathan De Lee ; Jason Eastman ; Massimiliano Esposito ; Scott W. Fleming ; B. Scott Gaudi ; Luan Ghezzi ; Jonay I. Gonzalez Hernandez ; Brian L. Lee ; Keivan G. Stassun ; Eric Agol ; Carlos Allende Prieto ; Rory Barnes ; Dmitry Bizyaev ; Phillip Cargile ; Liang Chang ; Luiz N. Da Costa ; G.F. Porto De Mello ; Bruno Femenia ; 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 ; Ricardo L.C. Ogando ; Daniel J. Oravetz ; Martin Paegert ; Kaike Pan ; Joshua Pepper ; Rafael Rebolo ; Basilio Santiago ; Donald P. Schneider ; Alaina C Shelden ; Audrey Simmons ; Benjamin M. Tofflemire ; Xiaoke Wan ; Ji Wang ; Bo Zhao ;
Date:	22 Feb 2012
Abstract:	TYC 4110-01037-1 has a low-mass stellar companion, whose small mass ratio and short orbital period are atypical amongst solar-like (Teff ~< 6000 K) binary systems. Our analysis of TYC 4110-01037-1 reveals it to be a moderately aged (~<5 Gyr) solar-like star having a mass of 1.07 +/- 0.08 MSun and radius of 0.99 +/- 0.18 RSun. We analyze 32 radial velocity measurements from the SDSS-III MARVELS survey as well as 6 supporting radial velocity measurements from the SARG spectrograph on the 3.6m TNG telescope obtained over a period of ~2 years. The best Keplerian orbital fit parameters were found to have a period of 78.994 +/- 0.012 days, an eccentricity of 0.1095 +/- 0.0023, and a semi-amplitude of 4199 +/- 11 m/s. We determine the minimum companion mass (if sin i = 1) to be 97.7 +/- 5.8 MJup. The system’s companion to host star mass ratio, >0.087 +/- 0.003, places it at the lowest end of observed values for short period stellar companions to solar-like (Teff ~< 6000 K) stars. One possible way to create such a system would be if a triple-component stellar multiple broke up into a short period, low q binary during the cluster dispersal phase of its lifetime. A candidate tertiary body has been identified in the system via single-epoch, high contrast imagery. If this object is confirmed to be co-moving, we estimate it would be a dM4 star. We present these results in the context of our larger-scale effort to constrain the statistics of low mass stellar and brown dwarf companions to FGK-type stars via the MARVELS survey.
Source:	arXiv, 1202.4964
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