  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.
