TY - JOUR
T1 - The Transiting Multi-planet System HD 3167
T2 - A 5.7 M ⊕ Super-Earth and an 8.3 M ⊕ Mini-Neptune
AU - Gandolfi, Davide
AU - Barragán, Oscar
AU - Hatzes, Artie P.
AU - Fridlund, Malcolm
AU - Fossati, Luca
AU - Donati, Paolo
AU - Johnson, Marshall C.
AU - Nowak, Grzegorz
AU - Prieto-Arranz, Jorge
AU - Albrecht, Simon
AU - Dai, Fei
AU - Deeg, Hans
AU - Endl, Michael
AU - Grziwa, Sascha
AU - Hjorth, Maria
AU - Korth, Judith
AU - Nespral, David
AU - Saario, Joonas
AU - Smith, Alexis M.S.
AU - Antoniciello, Giuliano
AU - Alarcon, Javier
AU - Bedell, Megan
AU - Blay, Pere
AU - Brems, Stefan S.
AU - Cabrera, Juan
AU - Csizmadia, Szilard
AU - Cusano, Felice
AU - Cochran, William D.
AU - Eigmüller, Philipp
AU - Erikson, Anders
AU - González Hernández, Jonay I.
AU - Guenther, Eike W.
AU - Hirano, Teruyuki
AU - Suárez Mascareño, Alejandro
AU - Narita, Norio
AU - Palle, Enric
AU - Parviainen, Hannu
AU - Pätzold, Martin
AU - Persson, Carina M.
AU - Rauer, Heike
AU - Saviane, Ivo
AU - Schmidtobreick, Linda
AU - Van Eylen, Vincent
AU - Winn, Joshua N.
AU - Zakhozhay, Olga V.
N1 - Funding Information:
This paper and the paper by Christiansen et al. (2017) were prepared simultaneously and are the result of independent RV observations and analyses of the HD 3167 system. We thank the anonymous referee for a thoughtful review and very positive feedback. We are extremely grateful to the NOT, ESO, and TNG staff members for their unique and superb support during the observations. We thank Xavier Bonfils, François Bouchy, Martin Kürster, Jorge Melendez, and Nuno Santos who kindly agreed to exchange HARPS time with us. D.G. would like to acknowledge the inspiring discussions with Conny Konnopke, Nuccio Lanza, Paul Robertson, Rodrigo Diaz, Elisa Delgado Mena, and Aldo Bonomo. D.G. gratefully acknowledges the financial support of the Programma Giovani Ricercatori—Rita Levi Montalcini— Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). M.F. and C.M.P. acknowledge generous support from the Swedish National Space Board. L.F. acknowledges the Austrian Forschungsförderungsge-sellschaft FFG project “TAPAS4CHEOPS” P853993. S.z.C. thanks the Hungarian OTKA Grant K113117. H.J.D. and D.N. acknowledge support from grant ESP2015-65712-C5-4-R of the Spanish Secretary of State for R& D&i (MINECO). This research was supported by the Ministerio de Economia y Competitividad under project FIS2012-31079. JIGH and ASM acknowledge financial support from the Spanish Ministry project MINECO AYA2014-56359-P, and J.I.G.H. also from the Spanish MINECO under the 2013 Ramón y Cajal program MINECO RYC-2013-14875. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/ 2013-2016) under grant agreement No. 312430 (OPTICON). Based on observations obtained (a) with the Nordic Optical Telescope (NOT), operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos (ORM) of the Instituto de Astrofísica de Canarias (IAC); (b) with the Italian Telescopio Nazionale Galileo (TNG) also operated at the ORM (IAC) on the island of La Palma by the INAF—Fundación Galileo Galilei; (c) the 3.6 m ESO telescope at La Silla Observatory under programs ID 097.C-0948 and 098.C-0860. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.
Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/9
Y1 - 2017/9
N2 - 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 +1.10 -0.98g 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 +1.79-1.85M ⊕ and a radius of 2.740 +0.106 -0.100 R ⊕, yielding a mean density of 2.21+0.56 -0.53g 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.
AB - 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 +1.10 -0.98g 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 +1.79-1.85M ⊕ and a radius of 2.740 +0.106 -0.100 R ⊕, yielding a mean density of 2.21+0.56 -0.53g 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.
KW - planets and satellites: detection
KW - planets and satellites: individual (HD 3167b, HD 3167c)
KW - stars: fundamental parameters
KW - stars: individual (HD 3167)
UR - http://www.scopus.com/inward/record.url?scp=85029085750&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85029085750&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/aa832a
DO - 10.3847/1538-3881/aa832a
M3 - Article
AN - SCOPUS:85029085750
SN - 0004-6256
VL - 154
JO - Astronomical Journal
JF - Astronomical Journal
IS - 3
M1 - 123
ER -