  We present the first resolved image of the debris disk around the 16+/-8 Myr
old star, HD 114082. The observation was made in the H-band using the SPHERE
instrument. The star is at a distance of 92+/-6 pc in the Lower Centaurus Crux
association. Using a Markov Chain Monte Carlo analysis, we determined that the
debris is likely in the form of a dust ring with an inner edge of 27.7+2.8/-3.5
au, position angle -74+0.5/-1.5 deg, and an inclination with respect to the
line of sight of 6.7+3.8/-0.4 deg. The disk imaged in scattered light has a
surface density declining with radius like ~r^(-4), steeper than expected for
grain blowout by radiation pressure. We find only marginal evidence (2 sigma)
of eccentricity, and rule out planets more massive than 1.0 Mjup orbiting
within 1 au of the ring's inner edge, since such a planet would have disrupted
the disk. The disk has roughly the same fractional disk luminosity
(Ldisk/L*=3.3x10^(-3)) as HR4796A and Beta Pictoris, however it was not
detected by previous instrument facilities most likely because of its small
angular size (radius~0.4"), low albedo (~0.2) and low scattering efficiency far
from the star due to high scattering anisotropy. With the arrival of extreme
adaptive optics systems like SPHERE and GPI, the morphology of smaller, fainter
and more distant debris disks are being revealed, providing clues to
planet-disk interactions in young protoplanetary systems.
