Bibcode
Esposito, M.; Armstrong, D. J.; Gandolfi, D.; Adibekyan, V.; Fridlund, M.; Santos, N. C.; Livingston, J. H.; Delgado Mena, E.; Fossati, L.; Lillo-Box, J.; Barragán, O.; Barrado, D.; Cubillos, P. E.; Cooke, B.; Justesen, A. B.; Meru, F.; Díaz, R. F.; Dai, F.; Nielsen, L. D.; Persson, C. M.; Wheatley, P. J.; Hatzes, A. P.; Van Eylen, V.; Musso, M. M.; Alonso, R.; Beck, P. G.; Barros, S. C. C.; Bayliss, D.; Bonomo, A. S.; Bouchy, F.; Brown, D. J. A.; Bryant, E.; Cabrera, J.; Cochran, W. D.; Csizmadia, S.; Deeg, H.; Demangeon, O.; Deleuil, M.; Dumusque, X.; Eigmüller, P.; Endl, M.; Erikson, A.; Faedi, F.; Figueira, P.; Fukui, A.; Grziwa, S.; Guenther, E. W.; Hidalgo, D.; Hjorth, M.; Hirano, T.; Hojjatpanah, S.; Knudstrup, E.; Korth, J.; Lam, K. W. F.; de Leon, J.; Lund, M. N.; Luque, R.; Mathur, S.; Montañés Rodríguez, P.; Narita, N.; Nespral, D.; Niraula, P.; Nowak, G.; Osborn, H. P.; Pallé, E.; Pätzold, M.; Pollacco, D.; Prieto-Arranz, J.; Rauer, H.; Redfield, S.; Ribas, I.; Sousa, S. G.; Smith, A. M. S.; Tala-Pinto, M.; Udry, S.; Winn, J. N.
Bibliographical reference
Astronomy and Astrophysics, Volume 623, id.A165, 11 pp.
Advertised on:
3
2019
Journal
Citations
31
Refereed citations
29
Description
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.
Based on observations made with the 3.6 m-ESO telescope at La Silla
observatory under ESO programmes IDs 1102.C-0923 (PI: Gandolfi) and
1102.C-0249 (PI: Armstrong).
Related projects
Helio and Astero-Seismology and Exoplanets Search
The principal objectives of this project are: 1) to study the structure and dynamics of the solar interior, 2) to extend this study to other stars, 3) to search for extrasolar planets using photometric methods (primarily by transits of their host stars) and their characterization (using radial velocity information) and 4) the study of the planetary
Savita
Mathur
Exoplanets and Astrobiology
The search for life in the universe has been driven by recent discoveries of planets around other stars (known as exoplanets), becoming one of the most active fields in modern astrophysics. The growing number of new exoplanets discovered in recent years and the recent advance on the study of their atmospheres are not only providing new valuable
Enric
Pallé Bago
Exoplanets and Astrobiology
The search for life in the universe has been driven by recent discoveries of planets around other stars (known as exoplanets), becoming one of the most active fields in modern astrophysics. The growing number of new exoplanets discovered in recent years and the recent advance on the study of their atmospheres are not only providing new valuable
Enric
Pallé Bago