Volume 647, March 2021
|Number of page(s)||10|
|Section||Planets and planetary systems|
|Published online||31 March 2021|
NGTS-13b: a hot 4.8 Jupiter-mass planet transiting a subgiant star★
Observatoire de Genève, Université de Genève,
Chemin Pegasi 51b,
2 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
3 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
4 Centre for Exoplanets and Habitability, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
5 Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489 Berlin, Germany
6 School of Physics and Astronomy, University of Leicester, LE1 7RH, UK
7 Center for Astronomy and Astrophysics, TU Berlin, Hardenbergstr. 36, 10623 Berlin, Germany
8 Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, UK
9 Astrophysics Group, Cavendish Laboratory, J.J. Thomson Avenue, Cambridge CB3 0HE, UK
10 Department of Physics, Kavli Institute for Astrophysics and Space Research, MIT, 77 Mass. Ave, Cambridge, MA 02139, USA
11 Centro de Astrofísica y Tecnologías Afines (CATA), Casilla 36-D, Santiago, Chile
12 Facultad de Ingeniería y Ciencias, Universidad Adolfo Ibáñez, Av. Diagonal las Torres 2640, Peñalolén, Santiago, Chile
13 Millennium Institute for Astrophysics, Santiago, Chile
14 Instituto de Astronomía, Universidad Católica del Norte, Angamos 0610, 1270709 Antofagasta, Chile
Accepted: 6 January 2021
We report the discovery of the massive hot Jupiter NGTS-13b by the Next Generation Transit Survey (NGTS). The V = 12.7 host star is likely in the subgiant evolutionary phase with logg* = 4.04 ± 0.05, Teff = 5819 ± 73 K, M* = 1.30−0.18+0.11 M⊙, and R* = 1.79 ± 0.06 R⊙. The NGTS detected a transiting planet with a period of P = 4.12 days around the star, which was later validated with the Transiting Exoplanet Survey Satellite (TESS; TIC 454069765). We confirm the planet using radial velocities from the CORALIE spectrograph. Using NGTS and TESS full-frame image photometry combined with CORALIE radial velocities, we determine NGTS-13b to have a radius of RP = 1.142 ± 0.046 RJup, a mass of MP = 4.84 ± 0.44 MJup, and an eccentricity of e = 0.086 ± 0.034. Previous studies have suggested that ~4 MJup may be the border separating two formation scenarios (e.g., core accretion and disk instability) and that massive giant planets share similar formation mechanisms as lower-mass brown dwarfs. NGTS-13b is just above 4 MJup, making it an important addition to the statistical sample needed to understand the differences between various classes of substellar companions. The high metallicity of NGTS-13, [Fe/H] = 0.25 ± 0.17, does not support previous suggestions that massive giants are found preferentially around lower metallicity host stars, but NGTS-13b does support findings that more massive and evolved hosts may have a higher occurrence of close-in massive planets than lower-mass unevolved stars.
Key words: planets and satellites: detection / planets and satellites: individual: NGTS-13b / techniques: photometric / techniques: radial velocities
NGTS and TESS reduced photometry files are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/647/A180
© ESO 2021
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