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korth

Judith Korth

Postdoc

korth

HD 219666 b : a hot-Neptune from TESS Sector 1

Author

  • M. Esposito
  • D. J. Armstrong
  • D. Gandolfi
  • V. Adibekyan
  • M. Fridlund
  • N. C. Santos
  • J. H. Livingston
  • E. Delgado Mena
  • L. Fossati
  • J. Lillo-Box
  • O. Barragán
  • D. Barrado
  • P. E. Cubillos
  • B. Cooke
  • A. B. Justesen
  • F. Meru
  • R. F. Díaz
  • F. Dai
  • L. D. Nielsen
  • C. M. Persson
  • P. J. Wheatley
  • A. P. Hatzes
  • V. Van Eylen
  • M. M. Musso
  • R. Alonso
  • P. G. Beck
  • S. C.C. Barros
  • D. Bayliss
  • A. S. Bonomo
  • F. Bouchy
  • D. J.A. Brown
  • E. Bryant
  • J. Cabrera
  • W. D. Cochran
  • S. Csizmadia
  • H. Deeg
  • O. Demangeon
  • M. Deleuil
  • X. Dumusque
  • P. Eigmüller
  • M. Endl
  • A. Erikson
  • F. Faedi
  • P. Figueira
  • A. Fukui
  • S. Grziwa
  • E. W. Guenther
  • D. Hidalgo
  • M. Hjorth
  • T. Hirano
  • S. Hojjatpanah
  • E. Knudstrup
  • J. Korth
  • K. W.F. Lam
  • J. De Leon
  • M. N. Lund
  • R. Luque
  • S. Mathur
  • P. Montañés Rodríguez
  • N. Narita
  • D. Nespral
  • P. Niraula
  • G. Nowak
  • H. P. Osborn
  • E. Pallé
  • M. Pätzold
  • D. Pollacco
  • J. Prieto-Arranz
  • H. Rauer
  • S. Redfield
  • I. Ribas
  • S. G. Sousa
  • A. M.S. Smith
  • M. Tala-Pinto
  • S. Udry
  • J. N. Winn
Show all

Summary, in English

We report on the confirmation and mass determination of a transiting planet orbiting the old and inactive G7 dwarf star HD 219666 (M∗ = 0.92 ± 0.03 M⊙, R∗ = 1.03 ± 0.03 R⊙, τ∗ = 10 ± 2 Gyr). With a mass of Mb = 16.6 ± 1.3 M⊙, a radius of Rb = 4.71 ± 0.17 R⊙, and an orbital period of Porb ≃ 6 days, HD 219666 b is a new member of a rare class of exoplanets: the hot-Neptunes. The Transiting Exoplanet Survey Satellite (TESS) observed HD 219666 (also known as TOI-118) in its Sector 1 and the light curve shows four transit-like events, equally spaced in time. We confirmed the planetary nature of the candidate by gathering precise radial-velocity measurements with the High Accuracy Radial velocity Planet Searcher (HARPS) at ESO 3.6 m. We used the co-added HARPS spectrum to derive the host star fundamental parameters (Teff = 5527 ± 65 K, log g∗ = 4.40 ± 0.11 (cgs), [Fe/H]= 0.04 ± 0.04 dex, log R′HK = -5.07 ± 0.03), as well as the abundances of many volatile and refractory elements. The host star brightness (V = 9.9) makes it suitable for further characterisation by means of in-transit spectroscopy. The determination of the planet orbital obliquity, along with the atmosphericmetal-to-hydrogen content and thermal structure could provide us with important clues on the formation mechanisms of this class of objects.

Publishing year

2019-03-01

Language

English

Publication/Series

Astronomy and Astrophysics

Volume

623

Document type

Journal article

Publisher

EDP Sciences

Keywords

  • Planets and satellites: detection
  • Planets and satellites: fundamental parameters
  • Planets and satellites: individual: HD 219666 b
  • Stars: fundamental parameters
  • Techniques: photometric
  • Techniques: radial velocities

Status

Published

ISBN/ISSN/Other

  • ISSN: 0004-6361