Volume 630, October 2019
|Number of page(s)||11|
|Section||Planets and planetary systems|
|Published online||24 September 2019|
INAF – Osservatorio Astronomico di Padova,
Vicolo dell’Osservatorio 5,
2 INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90134 Palermo, Italy
3 Dipartimento di Fisica e Astronomia – Universtà di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy
4 INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy
5 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese (TO), Italy
6 Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Clayton 3800, Melbourne, Australia
7 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany
8 INAF – Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy
9 INAF – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy
10 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
Accepted: 19 July 2019
Context. The origin of the observed diversity of planetary system architectures is one of the main topics of exoplanetary research. The detection of a statistically significant sample of planets around young stars allows us to study the early stages of planet formation and evolution, but only a handful are known so far. In this regard a considerable contribution is expected from the NASA TESS satellite, which is now performing a survey of ~85% of the sky to search for short-period transiting planets.
Aims. In its first month of operation TESS found a planet candidate with an orbital period of 8.14 days around a member of the Tuc-Hor young association (~40 Myr), the G6V main component of the binary system DS Tuc. If confirmed, it would be the first transiting planet around a young star suitable for radial velocity and/or atmospheric characterisation. Our aim is to validate the planetary nature of this companion and to measure its orbital and physical parameters.
Methods. We obtained accurate planet parameters by coupling an independent reprocessing of the TESS light curve with improved stellar parameters and the dilution caused by the binary companion; we analysed high-precision archival radial velocities to impose an upper limit of about 0.1 MJup on the planet mass; we finally ruled out the presence of external companions beyond 40 au with adaptive optics images.
Results. We confirm the presence of a young giant (R = 0.50 RJup) planet having a non-negligible possibility to be inflated (theoretical mass ≲ 20 M⊕) around DS Tuc A. We discuss the feasibility of mass determination, Rossiter-McLaughlin analysis, and atmosphere characterisation allowed by the brightness of the star.
Key words: planets and satellites: fundamental parameters / techniques: photometric / techniques: spectroscopic / techniques: radial velocities / techniques: imaging spectroscopy / stars: individual: DS Tuc A
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 075.C-0202(A), 0102.C-0618(A), 0103.C-0759(A), 075.A-9010(A), 076.A-9006(A), 073.C-0834(A), 083.C-0150(B).
© ESO 2019
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