The first scattered light images of HD 112810, a faint debris disk in the Sco-Cen association

¹ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
e-mail: matthews@mpia.de
² Department of Astronomy, University of Geneva, Chemin Pegasi 51, 1290 Versoix, Switzerland
³ Université Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
⁴ Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
⁵ INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
⁶ Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK Centre for Exoplanet Science, University of Edinburgh, Edinburgh EH9 3HJ, UK
⁷ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁸ Steward Observatory, Department of Astronomy, University of Arizona, 933 N. Cherry Ave, Tucson, AZ 85721, USA
⁹ LESIA, Observatoire de Paris, Université PSL, CNRS, Université Paris Cité, Sorbonne Université, 5 place Jules Janssen, 92195 Meudon, France
¹⁰ University of Exeter, Astrophysics Group, Physics Building, Stocker Road, Exeter EX4 4QL, UK
¹¹ School of Physics and Astronomy, Monash University, Vic 3800, Australia
¹² Jet Propulsion Laboratory, California Institute of Technology, Mail Stop 321-100, 4800 Oak Grove Drive, Pasadena, CA 91109, USA

Received: 3 July 2023
Accepted: 11 September 2023

Abstract

Context. Circumstellar debris disks provide insight into the formation and early evolution of planetary systems. Resolved belts in particular help to locate planetesimals in exosystems, and can hint at the presence of disk-sculpting exoplanets.

Aims. We study the circumstellar environment of HD 112810 (HIP 63439), a mid-F-type star in the Sco-Cen association with a significant infrared excess indicating the presence of a circumstellar debris disk.

Methods. We collected five high-contrast observations of HD 112810 with VLT/SPHERE. We identified a debris disk in scattered light, and found that the debris signature is robust over a number of epochs and a variety of reduction techniques. We modeled the disk, accounting for self-subtraction and assuming that it is optically thin.

Results. We find a single-belt debris disk, with a radius of 118 ± 9 au and an inclination angle of 75.7_−1.3^+1.1. This is in good agreement with the constraints from spectral energy distribution modeling and from a partially resolved ALMA image of the system. No planets are detected, though planets below the detection limit (~2.6 M_J at a projected separation of 118 au) could be present and could have contributed to sculpting the ring of debris.

Conclusions. HD 112810 adds to the growing inventory of debris disks imaged in scattered light. The disk is faint, but the radius and the inclination of the disk are promising for follow-up studies of the dust properties.