Very-low-mass stellar and substellar companion to solar-like stars from MARVELS. III. A short-period brown dwarf cadidate around an active G0IV subgiant

• Autor(a) principal: Ma, Bo
• Data de Publicação: 2013
• Outros Autores: Ge, Jian, Barnes, Rory, Crepp, Justin R., De Lee, Nathan M., Ferreira, Letícia D., Esposito, Massimiliano, Femenía Castellá, B., Fleming, S.W., Gaudi, B. S., Ghezzi, Luan, Hebb, Leslie, González Hernández, Jonay I., Lee, Brian L., Mello, Gustavo Frederico Porto de, Stassun, Keivan G., Wang, Ji, Wisniewski, J.P., Agol, Eric, Bizyaev, D., Cargile, Phillip A., Chang, Liang, Costa, Luiz N. da, Eastman, Jason, Gary, Bruce L., Jiang, Peng, Kane, Stephen R., Li, Rui, Liu, Jian, Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Muna, Demitri, Nguyen, D.C., Ogando, Ricardo L.C., Oravetz, Daniel J., Pepper, J., Paegert, Martin, Allende Prieto, Carlos, Rebolo, Rafael, Santiago, Basilio Xavier, Schneider, D.P., Bradley, Alaina C. Shelden, Simmons, Audrey E., Sivarani, Thirupathi, Van Eyken, Julian C., Wan, Xiaoke, Weaver, Benjamin A., Zhao, Bo
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/108145
• topic: Massa estelar; Movimento estelar; Anãs marrons; Brown dwarfs; Stars: low-mass; Techniques: radial velocities

We present an eccentric, short-period brown dwarf candidate orbiting the active, slightly evolved subgiant star TYC 2087-00255-1, which has effective temperature Teff = 5903±42 K, surface gravity log(g) = 4.07±0.16 (cgs), and metallicity [Fe/H] = −0.23 ± 0.07. This candidate was discovered using data from the first two years of the Multi-object APO Radial Velocity Exoplanets Large-area Survey, which is part of the third phase of Sloan Digital Sky Survey. From our 38 radial velocity measurements spread over a two-year time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 3.571 ± 0.041 km s−1, period P = 9.0090 ± 0.0004 days, and eccentricity e = 0.226±0.011. Adopting a mass of 1.16±0.11M for the subgiant host star, we infer that the companion has a minimum mass of 40.0 ± 2.5MJup. Assuming an edge-on orbit, the semimajor axis is 0.090 ± 0.003 AU. The host star is photometrically variable at the ∼1% level with a period of ∼13.16±0.01 days, indicating that the host star spin and companion orbit are not synchronized. Through adaptive optics imaging we also found a point source 643 ± 10 mas away from TYC 2087-00255-1, which would have a mass of 0.13M if it is physically associated with TYC 2087-00255-1 and has the same age. Future proper motion observation should be able to resolve if this tertiary object is physically associated with TYC 2087-00255-1 and make TYC 2087-00255-1 a triple body system. Core Ca ii H and K line emission indicate that the host is chromospherically active, at a level that is consistent with the inferred spin period and measured vrot sin i, but unusual for a subgiant of this Teff . This activity could be explained by ongoing tidal spin-up of the host star by the companion.