NGTS-13b: A hot 4.8 Jupiter-mass planet transiting a subgiant star

Nolan Grieves, Louise D. Nielsen, Jose I. Vines, Edward M. Bryant, Samuel Gill, François Bouchy, Monika Lendl, Daniel Bayliss, Philipp Eigmueller, Damien Segransan, Jack S. Acton, David R. Anderson, Matthew R. Burleigh, Sarah L. Casewell, Alexander Chaushev, Benjamin F. Cooke, Edward Gillen, Michael R. Goad, Maximilian N. Günther, Beth A. HendersonAleisha Hogan, James S. Jenkins, Douglas R. Alves, Andrés Jordán, James McCormac, Maximiliano Moyano, DIdier Queloz, Liam Raynard, Julia V. Seidel, Alexis M.S. Smith, Rosanna H. Tilbrook, Stephane Udry, Richard G. West, Peter J. Wheatley

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4 Citas (Scopus)

Resumen

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 Mpdbl, and R∗ = 1.79 ± 0.06 Rpdbl. 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.

Idioma originalInglés
Número de artículoA180
PublicaciónAstronomy and Astrophysics
Volumen647
DOI
EstadoPublicada - 1 mar. 2021
Publicado de forma externa

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