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

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. PerssonP. 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

Research output: Contribution to journalArticlepeer-review

14 Scopus citations

Abstract

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 RHK = -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.

Original languageEnglish (US)
Article numberA165
JournalAstronomy and Astrophysics
Volume623
DOIs
StatePublished - Mar 1 2019

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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

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