We present the first resolved image of the debris disk around the 16 \pm 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 \pm 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 -74.3 ^ { \circ } ^ { +0.5 } _ { -1.5 } , and an inclination with respect to the line of sight of 6.7 ^ { \circ } ^ { +3.8 } _ { -0.4 } .
The disk imaged in scattered light has a surface density that is declining with radius of \sim r ^ { -4 } , which is 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 M _ { Jup } orbiting within 1 au of the inner edge of the ring , since such a planet would have disrupted the disk .
The disk has roughly the same fractional disk luminosity ( L _ { disk } / L _ { * } =3.3 \times 10 ^ { -3 } ) as HR 4796 A and \beta Pictoris , however it was not detected by previous instrument facilities most likely because of its small angular size ( radius \sim 0.4 ^ { \prime \prime } ) , low albedo ( \sim 0.2 ) , and low scattering efficiency far from the star due to high scattering anisotropy .
With the arrival of extreme adaptive optics systems , such as 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 . Accepted by A & A on 7 November 2016 .