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25 April 2024 |
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Very Low-mass Stellar and Substellar Companions to Solar-like Stars from Marvels Iii: A Short-Period Brown Dwarf Candidate Around An Active G0Iv Subgiant | | Bo Ma
; Jian Ge
; Rory Barnes
; Justin R. Crepp
; Nathan De Lee
; Leticia Dutra-Ferreira
; Massimiliano Esposito
; Bruno Femenia
; Scott W. Fleming
; B. Scott Gaudi
; Luan Ghezzi
; Leslie Hebb
; Jonay I. Gonzalez Hernandez
; Brian L. Lee
; G. F. Porto de Mello
; Keivan G. Stassun
; Ji Wang
; John P. Wisniewski
; Eric Agol
; Dmitry Bizyaev
; Phillip Cargile
; Liang Chang
; Luiz Nicolaci da Costa
; Jason D. Eastman
; Bruce Gary
; Peng Jiang
; Stephen R. Kane
; Rui Li
; Jian Liu
; Suvrath Mahadevan
; Marcio A. G. Maia
; Demitri Muna
; Duy Cuong Nguyen
; Ricardo L. C. Ogando
; Daniel Oravetz
; Joshua Pepper
; Martin Paegert
; Carlos Allende Prieto
; Rafael Rebolo
; Basilio X. Santiago
; Donald P. Schneider
; Alaina Shelden
; Audrey Simmons
; Thirupathi Sivarani
; J. C. van Eyken
; Xiaoke Wan
; Benjamin A. Weaver
; Bo Zhao
; | | Date: |
26 Nov 2012 | | Abstract: | We present an eccentric, short-period brown dwarf candidate orbiting the
active, slightly evolved subgiant star TYC 2087-00255-1, which has effective
temperature T_eff = 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 (MARVELS), 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, period P=9.0090+/-0.0004 days, and eccentricity
e=0.226+/-0.011. Adopting a mass of 1.16+/-0.11 Msun for the subgiant host
star, we infer that the companion has a minimum mass of 40.0+/-2.5 M_Jup.
Assuming an edge-on orbit, the semimajor axis is 0.090+/-0.003 AU. The host
star is photometrically variable at the sim1% level with a period of
sim13.16+/-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 0.13
Msun 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 v_{rot}*sin i, but unusual for a subgiant of this
T_eff. This activity could be explained by ongoing tidal spin-up of the host
star by the companion. | | Source: | arXiv, 1211.6140 | | Services: | Forum | Review | PDF | Favorites | |
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