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HD219666b: 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. Persson
; P.J. Wheatley
; A.P. Hatzes
; V. Van Eylen
; M.M. Musso
; R. Alonso
; P. 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
; | | Date: |
14 Dec 2018 | | Abstract: | We report the discovery of a transiting planet orbiting the old and inactive
G7 dwarf star HD219666 (Mstar = 0.92 +/- 0.03 MSun, Rstar = 1.03 +/- 0.03 RSun,
tau_star = 10 +/- 2 Gyr). With a mass of Mb = 16.6 +/- 1.3 MEarth, a radius of
Rb = 4.71 +/- 0.17 REarth, and an orbital period of P ~ 6 days, HD219666b is a
new member of a rare class of exoplanets: the hot-Neptunes. The Transiting
Exoplanet Survey Satellite (TESS) observed HD219666 (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 HARPS@ESO3.6m. 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
characterization by means of in-transit spectroscopy. The determination of the
planet orbital obliquity, along with the atmospheric metal-to-hydrogen content
and thermal structure could provide us with important clues on the mechanisms
of formation of this class of objects. | | Source: | arXiv, 1812.5881 | | Services: | Forum | Review | PDF | Favorites | |
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