Bibcode
Gandolfi, D.; Barragán, Oscar; Hatzes, Artie P.; Fridlund, Malcolm; Fossati, Luca; Donati, Paolo; Johnson, Marshall C.; Nowak, G.; Prieto-Arranz, J.; Albrecht, Simon; Dai, Fei; Deeg, H. J.; Endl, Michael; Grziwa, Sascha; Hjorth, Maria; Korth, Judith; Nespral, D.; Saario, Joonas; Smith, Alexis M. S.; Antoniciello, Giuliano; Alarcon, Javier; Bedell, Megan; Blay, P.; Brems, Stefan S.; Cabrera, Juan; Csizmadia, Szilard; Cusano, Felice; Cochran, William D.; Eigmüller, Philipp; Erikson, Anders; González Hernández, J. I.; Guenther, Eike W.; Hirano, Teruyuki; Suárez Mascareño, A.; Narita, Norio; Palle, E.; Parviainen, H.; Pätzold, Martin; Persson, Carina M.; Rauer, Heike; Saviane, Ivo; Schmidtobreick, Linda; Van Eylen, Vincent; Winn, Joshua N.; Zakhozhay, Olga V.
Referencia bibliográfica
The Astronomical Journal, Volume 154, Issue 3, article id. 123, 15 pp. (2017).
Fecha de publicación:
9
2017
Número de citas
56
Número de citas referidas
52
Descripción
HD 3167 is a bright (V = 8.9 mag) K0 V star observed by NASA’s K2
space mission during its Campaign 8. It has recently been found to host
two small transiting planets, namely, HD 3167b, an ultra-short-period
(0.96 days) super-Earth, and HD 3167c, a mini-Neptune on a relatively
long-period orbit (29.85 days). Here we present an intensive radial
velocity (RV) follow-up of HD 3167 performed with the FIES@NOT,
HARPS@ESO-3.6 m, and HARPS-N@TNG spectrographs. We revise the system
parameters and determine radii, masses, and densities of the two
transiting planets by combining the K2 photometry with our spectroscopic
data. With a mass of 5.69 ± 0.44 M ⊕, a radius
of 1.574 ± 0.054 R ⊕, and a mean density of
{8.00}-0.98+1.10 {{g}} {{cm}}-3, HD
3167b joins the small group of ultra-short-period planets known to have
rocky terrestrial compositions. HD 3167c has a mass of
{8.33}-1.85+1.79 M ⊕ and a radius
of {2.740}-0.100+0.106 R ⊕,
yielding a mean density of {2.21}-0.53+0.56 {{g}}
{{cm}}-3, indicative of a planet with a composition
comprising a solid core surrounded by a thick atmospheric envelope. The
rather large pressure scale height (∼350 km) and the brightness of
the host star make HD 3167c an ideal target for atmospheric
characterization via transmission spectroscopy across a broad range of
wavelengths. We found evidence of additional signals in the RV
measurements but the currently available data set does not allow us to
draw any firm conclusions on the origin of the observed variation.
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