Volume 655, November 2021
|Number of page(s)||12|
|Section||Planets and planetary systems|
|Published online||23 November 2021|
Univ. Grenoble Alpes, CNRS, IPAG,
2 LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, Université Pierre et Marie Curie, 5 place Jules Janssen, 92190 Meudon, France
3 SUPA, Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
4 Centre for Exoplanet Science, University of Edinburgh, Edinburgh, UK
5 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France
6 Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMI 3386 and Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
7 INAF - Osservatorio Astronomico di Padova, Vicolo della Osservatorio 5, 35122, Padova, Italy
8 Steward Observatory, Department of Astronomy, University of Arizona, 933 N. Cherry Ave, Tucson, AZ 85721, USA
9 University of Exeter, School of Physics & Astronomy, Stocker Road, Exeter EX4 4QL, UK
10 Dipartimento di Fisica a Astronomia “G. Galilei”, Universita di Padova, Via Marzolo, 8, 35121 Padova, Italy
11 Observatoire de l’Université de Genève, Chemin Pegasi 51, 1290 Versoix, Switzerland
12 Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA02139, USA
13 Physikalisches Institut, University of Bern, Gesellschaftsstrasse 6, 3012 Bern, Switzerland
14 Núcleo Milenio Formación Planetaria - NPF, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile
15 School of Physics and Astronomy, Monash University, Clayton, Vic 3800, Australia
Accepted: 22 October 2021
Context. We initiated a deep-imaging survey of Scorpius-Centaurus A-F stars in 2015. These stars are predicted to host warm inner and cold outer belts of debris reminiscent of the architecture of emblematic systems such as HR 8799.
Aims. We present resolved images of a ring of debris around the F5-type star HD 141011 that was observed as part of our survey. We aim to set constraints on the properties of the disk, compare them to those of other resolved debris disks in Sco-Cen, and detect companions.
Methods. We obtained high-contrast coronagraphic observations of HD 141011 in 2015, 2016, and 2019 with VLT/SPHERE. We removed the stellar halo using angular differential imaging. We searched for scattered light emission from a disk in the residuals and applied a forward-modeling approach to retrieve its morphological and photometric properties. We combined our radial velocity and imaging data to derive detection probabilities for companions co-planar with the disk orientation.
Results. We resolve a narrow ring of debris that extends up to ~1.1″ (~141 au) from the star in the IRDIS and IFS data obtained in 2016 and 2019. The disk is not detected in the 2015 data which are of poorer quality. The disks is best reproduced by models of a noneccentric ring centered on the star with an inclination of 69.1 ± 0.9°, a position angle of −24.6 ± 1.7°, and a semimajor axis of 127.5 ± 3.8 au. The combination of radial velocity and imaging data excludes brown-dwarf (M > 13.6MJup) companions coplanar with the disk from 0.1 to 0.9 au and from 20 au up to 500 au (90% probability).
Conclusions. HD 141011 adds to the growing list of debris disks that are resolved in Sco-Cen. It is one of the faintest disks that are resolved from the ground and has a radial extent and fractional width (~12.5%) reminiscent of Fomalhaut. Its moderate inclination and large semimajor axis make it a good target for the James Webb Space Telescope and should allow a deeper search for putative companions shaping the dust distribution.
Key words: techniques: high angular resolution / planetary systems / stars: individual: HD 141011 (HIP 77432) / stars: imaging
Based on observations made with ESO Telescopes at the Paranal Observatory under programs ID 095.C-0607, 097.C-0060, 0101.C-0016, 098.C-0739, and 1101.C-0557.
© M. Bonnefoy et al. 2021
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