The SHARDDS survey: First resolved image of the HD 114082 debris disk in the Lower Centaurus Crux with SPHERE ^⋆

¹ European Southern Observatory, Alonso de Còrdova 3107, Vitacura, Casilla 19001, Santiago, Chile
e-mail: zwahhaj@eso.org
² Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
³ Steward Observatory, Department of Astronomy, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA
⁴ LESIA, Observatoire de Paris, PSL Research Univ., CNRS, Sorbonne Univ., UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 92195 Meudon, France
⁵ Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro 1, Sta. Ma. Tonantzintla, Puebla, Mexico
⁶ UMI-FCA, CNRS/INSU (UMI 3386), France
⁷ Dept. de Astronomía, Universidad de Chile, Santiago, Chile
⁸ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
⁹ STAR Institute, Université de Liège, 19c Allée du Six Août, 4000 Liège, Belgium
¹⁰ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
¹¹ Hubble Fellow at Jet Propulsion Laboratory, Caltech, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
¹² Department of Physics, Nagoya University, Nagoya, Aichi 464-8602, Japan
¹³ Dept. of Astronomy, California Institute of Technology, 1200 E. CA Boulevard, Pasadena, CA 91125, USA
¹⁴ ALMA Santiago Central Offices, Alonso de Còrdova 3107, Vitacura, Casilla 763 0355, Santiago, Chile

Received: 21 September 2016
Accepted: 7 November 2016

Abstract

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 –74.3°^+0.5_-1.5, and an inclination with respect to the line of sight of 6.7°^+3.8_-0.4. The disk imaged in scattered light has a surface density that is declining with radius of ~r^-4, which is steeper than expected for grain blowout by radiation pressure. We find only marginal evidence (2σ) 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 × 10^-3) as HR 4796 A and β 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, 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.