The Transiting Multi-planet System HD 3167: A 5.7 M ⊕ Super-Earth and an 8.3 M ⊕ Mini-Neptune

Davide Gandolfi; Oscar Barragán; Artie P. Hatzes; Malcolm Fridlund; Luca Fossati; Paolo Donati; Marshall C. Johnson; Grzegorz Nowak; Jorge Prieto-Arranz; Simon Albrecht; Fei Dai; Hans Deeg; Michael Endl; Sascha Grziwa; Maria Hjorth; Judith Korth; David Nespral; Joonas Saario; Alexis M.S. Smith; Giuliano Antoniciello; Javier Alarcon; Megan Bedell; Pere Blay; Stefan S. Brems; Juan Cabrera; Szilard Csizmadia; Felice Cusano; William D. Cochran; Philipp Eigmüller; Anders Erikson; Jonay I. González Hernández; Eike W. Guenther; Teruyuki Hirano; Alejandro Suárez Mascareño; Norio Narita; Enric Palle; Hannu Parviainen; Martin Pätzold; Carina M. Persson; Heike Rauer; Ivo Saviane; Linda Schmidtobreick; Vincent Van Eylen; Joshua N. Winn; Olga V. Zakhozhay

doi:10.3847/1538-3881/aa832a

The Transiting Multi-planet System HD 3167: A 5.7 M _⊕ Super-Earth and an 8.3 M _⊕ Mini-Neptune

Davide Gandolfi, Oscar Barragán, Artie P. Hatzes, Malcolm Fridlund, Luca Fossati, Paolo Donati, Marshall C. Johnson, Grzegorz Nowak, Jorge Prieto-Arranz, Simon Albrecht, Fei Dai, Hans Deeg, Michael Endl, Sascha Grziwa, Maria Hjorth, Judith Korth, David Nespral, Joonas Saario, Alexis M.S. Smith, Giuliano AntonicielloJavier Alarcon, Megan Bedell, Pere Blay, Stefan S. Brems, Juan Cabrera, Szilard Csizmadia, Felice Cusano, William D. Cochran, Philipp Eigmüller, Anders Erikson, Jonay I. González Hernández, Eike W. Guenther, Teruyuki Hirano, Alejandro Suárez Mascareño, Norio Narita, Enric Palle, Hannu Parviainen, Martin Pätzold, Carina M. Persson, Heike Rauer, Ivo Saviane, Linda Schmidtobreick, Vincent Van Eylen, Joshua N. Winn, Olga V. Zakhozhay

Astrophysical Sciences

Research output: Contribution to journal › Article › peer-review

47 Scopus citations

Abstract

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.

Original language	English (US)
Article number	123
Journal	Astronomical Journal
Volume	154
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aa832a
State	Published - Sep 2017

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

planets and satellites: detection
planets and satellites: individual (HD 3167b, HD 3167c)
stars: fundamental parameters
stars: individual (HD 3167)

Access to Document

10.3847/1538-3881/aa832a

Cite this

Gandolfi, D., Barragán, O., Hatzes, A. P., Fridlund, M., Fossati, L., Donati, P., Johnson, M. C., Nowak, G., Prieto-Arranz, J., Albrecht, S., Dai, F., Deeg, H., Endl, M., Grziwa, S., Hjorth, M., Korth, J., Nespral, D., Saario, J., Smith, A. M. S., ... Zakhozhay, O. V. (2017). The Transiting Multi-planet System HD 3167: A 5.7 M _⊕ Super-Earth and an 8.3 M _⊕ Mini-Neptune. Astronomical Journal, 154(3), Article 123. https://doi.org/10.3847/1538-3881/aa832a

@article{6900eca0e2774820a9a669748068816a,

title = "The Transiting Multi-planet System HD 3167: A 5.7 M ⊕ Super-Earth and an 8.3 M ⊕ Mini-Neptune",

abstract = "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.",

keywords = "planets and satellites: detection, planets and satellites: individual (HD 3167b, HD 3167c), stars: fundamental parameters, stars: individual (HD 3167)",

author = "Davide Gandolfi and Oscar Barrag{\'a}n and Hatzes, {Artie P.} and Malcolm Fridlund and Luca Fossati and Paolo Donati and Johnson, {Marshall C.} and Grzegorz Nowak and Jorge Prieto-Arranz and Simon Albrecht and Fei Dai and Hans Deeg and Michael Endl and Sascha Grziwa and Maria Hjorth and Judith Korth and David Nespral and Joonas Saario and Smith, {Alexis M.S.} and Giuliano Antoniciello and Javier Alarcon and Megan Bedell and Pere Blay and Brems, {Stefan S.} and Juan Cabrera and Szilard Csizmadia and Felice Cusano and Cochran, {William D.} and Philipp Eigm{\"u}ller and Anders Erikson and {Gonz{\'a}lez Hern{\'a}ndez}, {Jonay I.} and Guenther, {Eike W.} and Teruyuki Hirano and {Su{\'a}rez Mascare{\~n}o}, Alejandro and Norio Narita and Enric Palle and Hannu Parviainen and Martin P{\"a}tzold and Persson, {Carina M.} and Heike Rauer and Ivo Saviane and Linda Schmidtobreick and {Van Eylen}, Vincent and Winn, {Joshua N.} and Zakhozhay, {Olga V.}",

note = "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, Fran{\c c}ois Bouchy, Martin K{\"u}rster, 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 Forschungsf{\"o}rderungsge-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 Ram{\'o}n 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 Astrof{\'i}sica 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—Fundaci{\'o}n 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: {\textcopyright} 2017. The American Astronomical Society. All rights reserved.",

year = "2017",

month = sep,

doi = "10.3847/1538-3881/aa832a",

language = "English (US)",

volume = "154",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "3",

}

Gandolfi, D, Barragán, O, Hatzes, AP, Fridlund, M, Fossati, L, Donati, P, Johnson, MC, Nowak, G, Prieto-Arranz, J, Albrecht, S, Dai, F, Deeg, H, Endl, M, Grziwa, S, Hjorth, M, Korth, J, Nespral, D, Saario, J, Smith, AMS, Antoniciello, G, Alarcon, J, Bedell, M, Blay, P, Brems, SS, Cabrera, J, Csizmadia, S, Cusano, F, Cochran, WD, Eigmüller, P, Erikson, A, González Hernández, JI, Guenther, EW, Hirano, T, Suárez Mascareño, A, Narita, N, Palle, E, Parviainen, H, Pätzold, M, Persson, CM, Rauer, H, Saviane, I, Schmidtobreick, L, Van Eylen, V, Winn, JN & Zakhozhay, OV 2017, 'The Transiting Multi-planet System HD 3167: A 5.7 M _⊕ Super-Earth and an 8.3 M _⊕ Mini-Neptune', Astronomical Journal, vol. 154, no. 3, 123. https://doi.org/10.3847/1538-3881/aa832a

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)

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JF - Astronomical Journal

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