Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

Jessie L. Christiansen; Andrew Vanderburg; Jennifer Burt; B. J. Fulton; Konstantin Batygin; Björn Benneke; John M. Brewer; David Charbonneau; David R. Ciardi; Andrew Collier Cameron; Jeffrey L. Coughlin; Ian J.M. Crossfield; Courtney Dressing; Thomas P. Greene; Andrew W. Howard; David W. Latham; Emilio Molinari; Annelies Mortier; Fergal Mullally; Francesco Pepe; Ken Rice; Evan Sinukoff; Alessandro Sozzetti; Susan E. Thompson; Stéphane Udry; Steven S. Vogt; Travis S. Barman; Natasha E. Batalha; François Bouchy; Lars A. Buchhave; R. Paul Butler; Rosario Cosentino; Trent J. Dupuy; David Ehrenreich; Aldo Fiorenzano; Brad M.S. Hansen; Thomas Henning; Lea Hirsch; Bradford P. Holden; Howard T. Isaacson; John A. Johnson; Heather A. Knutson; Molly Kosiarek; Mercedes López-Morales; Christophe Lovis; Luca Malavolta; Michel Mayor; Giuseppina Micela; Fatemeh Motalebi; Erik Petigura; David F. Phillips; Giampaolo Piotto; Leslie A. Rogers; Dimitar Sasselov; Joshua E. Schlieder; Damien Ségransan; Christopher A. Watson; Lauren M. Weiss

doi:10.3847/1538-3881/aa832d

Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

Jessie L. Christiansen, Andrew Vanderburg, Jennifer Burt, B. J. Fulton, Konstantin Batygin, Björn Benneke, John M. Brewer, David Charbonneau, David R. Ciardi, Andrew Collier Cameron, Jeffrey L. Coughlin, Ian J.M. Crossfield, Courtney Dressing, Thomas P. Greene, Andrew W. Howard, David W. Latham, Emilio Molinari, Annelies Mortier, Fergal Mullally, Francesco PepeKen Rice, Evan Sinukoff, Alessandro Sozzetti, Susan E. Thompson, Stéphane Udry, Steven S. Vogt, Travis S. Barman, Natasha E. Batalha, François Bouchy, Lars A. Buchhave, R. Paul Butler, Rosario Cosentino, Trent J. Dupuy, David Ehrenreich, Aldo Fiorenzano, Brad M.S. Hansen, Thomas Henning, Lea Hirsch, Bradford P. Holden, Howard T. Isaacson, John A. Johnson, Heather A. Knutson, Molly Kosiarek, Mercedes López-Morales, Christophe Lovis, Luca Malavolta, Michel Mayor, Giuseppina Micela, Fatemeh Motalebi, Erik Petigura, David F. Phillips, Giampaolo Piotto, Leslie A. Rogers, Dimitar Sasselov, Joshua E. Schlieder, Damien Ségransan, Christopher A. Watson, Lauren M. Weiss

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

62 Scopus citations

Abstract

HD 3167 is a bright (V = 8.9), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 ±0.38 M₊for HD 3167 b, a hot super-Earth with a likely rocky composition (ρb = 5.60 ^+2.15 _-1.43= g cm^-3), and 9.80 ^+1.30 _-1.24 M₊for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (p_c = 1.97 ^0.94 _-0.59 g cm^-3). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 ±0.045 d (between planets b and c) and a minimum mass of 6.90 ±0.71 M_⊕. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.°3 because we do not observe transits of planet d. From 1.°3 to 40°, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40° to 60°, Kozai-Lidov oscillations increase the system's instability, but it can remain stable for up to 100 Myr. Above 60°, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission.

Original language	English (US)
Article number	122
Journal	Astronomical Journal
Volume	154
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aa832d
State	Published - Sep 2017

Keywords

eclipses
stars: individual (HD 3167)
techniques: photometric
techniques: spectroscopic

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-3881/aa832d

Cite this

Christiansen, J. L., Vanderburg, A., Burt, J., Fulton, B. J., Batygin, K., Benneke, B., Brewer, J. M., Charbonneau, D., Ciardi, D. R., Cameron, A. C., Coughlin, J. L., Crossfield, I. J. M., Dressing, C., Greene, T. P., Howard, A. W., Latham, D. W., Molinari, E., Mortier, A., Mullally, F., ... Weiss, L. M. (2017). Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets. Astronomical Journal, 154(3), [122]. https://doi.org/10.3847/1538-3881/aa832d

Christiansen, JL, Vanderburg, A, Burt, J, Fulton, BJ, Batygin, K, Benneke, B, Brewer, JM, Charbonneau, D, Ciardi, DR, Cameron, AC, Coughlin, JL, Crossfield, IJM, Dressing, C, Greene, TP, Howard, AW, Latham, DW, Molinari, E, Mortier, A, Mullally, F, Pepe, F, Rice, K, Sinukoff, E, Sozzetti, A, Thompson, SE, Udry, S, Vogt, SS, Barman, TS, Batalha, NE, Bouchy, F, Buchhave, LA, Butler, RP, Cosentino, R, Dupuy, TJ, Ehrenreich, D, Fiorenzano, A, Hansen, BMS, Henning, T, Hirsch, L, Holden, BP, Isaacson, HT, Johnson, JA, Knutson, HA, Kosiarek, M, López-Morales, M, Lovis, C, Malavolta, L, Mayor, M, Micela, G, Motalebi, F, Petigura, E, Phillips, DF, Piotto, G, Rogers, LA, Sasselov, D, Schlieder, JE, Ségransan, D, Watson, CA & Weiss, LM 2017, 'Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets', Astronomical Journal, vol. 154, no. 3, 122. https://doi.org/10.3847/1538-3881/aa832d

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title = "Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets",

abstract = "HD 3167 is a bright (V = 8.9), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 ±0.38 M+for HD 3167 b, a hot super-Earth with a likely rocky composition (ρb = 5.60 +2.15 -1.43= g cm-3), and 9.80 +1.30 -1.24 M+for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (pc = 1.97 0.94 -0.59 g cm-3). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 ±0.045 d (between planets b and c) and a minimum mass of 6.90 ±0.71 M⊕. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.°3 because we do not observe transits of planet d. From 1.°3 to 40°, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40° to 60°, Kozai-Lidov oscillations increase the system's instability, but it can remain stable for up to 100 Myr. Above 60°, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission.",

keywords = "eclipses, stars: individual (HD 3167), techniques: photometric, techniques: spectroscopic",

author = "Christiansen, {Jessie L.} and Andrew Vanderburg and Jennifer Burt and Fulton, {B. J.} and Konstantin Batygin and Bj{\"o}rn Benneke and Brewer, {John M.} and David Charbonneau and Ciardi, {David R.} and Cameron, {Andrew Collier} and Coughlin, {Jeffrey L.} and Crossfield, {Ian J.M.} and Courtney Dressing and Greene, {Thomas P.} and Howard, {Andrew W.} and Latham, {David W.} and Emilio Molinari and Annelies Mortier and Fergal Mullally and Francesco Pepe and Ken Rice and Evan Sinukoff and Alessandro Sozzetti and Thompson, {Susan E.} and St{\'e}phane Udry and Vogt, {Steven S.} and Barman, {Travis S.} and Batalha, {Natasha E.} and Fran{\c c}ois Bouchy and Buchhave, {Lars A.} and Butler, {R. Paul} and Rosario Cosentino and Dupuy, {Trent J.} and David Ehrenreich and Aldo Fiorenzano and Hansen, {Brad M.S.} and Thomas Henning and Lea Hirsch and Holden, {Bradford P.} and Isaacson, {Howard T.} and Johnson, {John A.} and Knutson, {Heather A.} and Molly Kosiarek and Mercedes L{\'o}pez-Morales and Christophe Lovis and Luca Malavolta and Michel Mayor and Giuseppina Micela and Fatemeh Motalebi and Erik Petigura and Phillips, {David F.} and Giampaolo Piotto and Rogers, {Leslie A.} and Dimitar Sasselov and Schlieder, {Joshua E.} and Damien S{\'e}gransan and Watson, {Christopher A.} and Weiss, {Lauren M.}",

note = "Funding Information: This paper and the paper by Gandolfi et al. were prepared simultaneously and are the result of independent radial-velocity observations and analyses of the HD3167 system. We thank the HARPS team for their collegiality. We also thank the many observers who contributed to the measurements reported here. We thank Kyle Lanclos, Matt Radovan, Will Deich, and the rest of the UCO Lick staff for their invaluable help shepherding, planning, and executing observations, in addition to writing the low-level software that made the automated APF observations possible. We are grateful to the time assignment committees of the University of Hawai{\textquoteright}i, the University of California, and NASA for their generous allocations of observing time. A.W.H. acknowledges support for our K2 team through a NASA Astrophysics Data Analysis Program grant. A.W.H. and I.J.M.C. acknowledge support from the K2 Guest Observer Program. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. Any opinion, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. The research leading to these results has received funding from the European Union Seventh Framework Program (FP7/ 2007–2013) under grant agreement number 313014 (ETAEARTH). This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by NASA under grant Nos. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has also made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This research has made use of the NASA Exoplanet Follow-Up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Finally, the authors wish to extend special thanks to those of Hawai{\textquoteright}ian ancestry on whose sacred mountain of Maunakea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. Facilities: Kepler, Keck(HIRES, NIRC2), APF, TNG. Publisher Copyright: {\textcopyright} 2017. The American Astronomical Society. All rights reserved.",

year = "2017",

month = sep,

doi = "10.3847/1538-3881/aa832d",

language = "English (US)",

volume = "154",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "3",

}

TY - JOUR

T1 - Three's Company

T2 - An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

AU - Christiansen, Jessie L.

AU - Vanderburg, Andrew

AU - Burt, Jennifer

AU - Fulton, B. J.

AU - Batygin, Konstantin

AU - Benneke, Björn

AU - Brewer, John M.

AU - Charbonneau, David

AU - Ciardi, David R.

AU - Cameron, Andrew Collier

AU - Coughlin, Jeffrey L.

AU - Crossfield, Ian J.M.

AU - Dressing, Courtney

AU - Greene, Thomas P.

AU - Howard, Andrew W.

AU - Latham, David W.

AU - Molinari, Emilio

AU - Mortier, Annelies

AU - Mullally, Fergal

AU - Pepe, Francesco

AU - Rice, Ken

AU - Sinukoff, Evan

AU - Sozzetti, Alessandro

AU - Thompson, Susan E.

AU - Udry, Stéphane

AU - Vogt, Steven S.

AU - Barman, Travis S.

AU - Batalha, Natasha E.

AU - Bouchy, François

AU - Buchhave, Lars A.

AU - Butler, R. Paul

AU - Cosentino, Rosario

AU - Dupuy, Trent J.

AU - Ehrenreich, David

AU - Fiorenzano, Aldo

AU - Hansen, Brad M.S.

AU - Henning, Thomas

AU - Hirsch, Lea

AU - Holden, Bradford P.

AU - Isaacson, Howard T.

AU - Johnson, John A.

AU - Knutson, Heather A.

AU - Kosiarek, Molly

AU - López-Morales, Mercedes

AU - Lovis, Christophe

AU - Malavolta, Luca

AU - Mayor, Michel

AU - Micela, Giuseppina

AU - Motalebi, Fatemeh

AU - Petigura, Erik

AU - Phillips, David F.

AU - Piotto, Giampaolo

AU - Rogers, Leslie A.

AU - Sasselov, Dimitar

AU - Schlieder, Joshua E.

AU - Ségransan, Damien

AU - Watson, Christopher A.

AU - Weiss, Lauren M.

N1 - Funding Information: This paper and the paper by Gandolfi et al. were prepared simultaneously and are the result of independent radial-velocity observations and analyses of the HD3167 system. We thank the HARPS team for their collegiality. We also thank the many observers who contributed to the measurements reported here. We thank Kyle Lanclos, Matt Radovan, Will Deich, and the rest of the UCO Lick staff for their invaluable help shepherding, planning, and executing observations, in addition to writing the low-level software that made the automated APF observations possible. We are grateful to the time assignment committees of the University of Hawai’i, the University of California, and NASA for their generous allocations of observing time. A.W.H. acknowledges support for our K2 team through a NASA Astrophysics Data Analysis Program grant. A.W.H. and I.J.M.C. acknowledge support from the K2 Guest Observer Program. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. Any opinion, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. The research leading to these results has received funding from the European Union Seventh Framework Program (FP7/ 2007–2013) under grant agreement number 313014 (ETAEARTH). This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by NASA under grant Nos. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has also made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This research has made use of the NASA Exoplanet Follow-Up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Finally, the authors wish to extend special thanks to those of Hawai’ian ancestry on whose sacred mountain of Maunakea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. Facilities: Kepler, Keck(HIRES, NIRC2), APF, TNG. 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), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 ±0.38 M+for HD 3167 b, a hot super-Earth with a likely rocky composition (ρb = 5.60 +2.15 -1.43= g cm-3), and 9.80 +1.30 -1.24 M+for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (pc = 1.97 0.94 -0.59 g cm-3). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 ±0.045 d (between planets b and c) and a minimum mass of 6.90 ±0.71 M⊕. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.°3 because we do not observe transits of planet d. From 1.°3 to 40°, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40° to 60°, Kozai-Lidov oscillations increase the system's instability, but it can remain stable for up to 100 Myr. Above 60°, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission.

AB - HD 3167 is a bright (V = 8.9), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 ±0.38 M+for HD 3167 b, a hot super-Earth with a likely rocky composition (ρb = 5.60 +2.15 -1.43= g cm-3), and 9.80 +1.30 -1.24 M+for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (pc = 1.97 0.94 -0.59 g cm-3). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 ±0.045 d (between planets b and c) and a minimum mass of 6.90 ±0.71 M⊕. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.°3 because we do not observe transits of planet d. From 1.°3 to 40°, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40° to 60°, Kozai-Lidov oscillations increase the system's instability, but it can remain stable for up to 100 Myr. Above 60°, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission.

KW - eclipses

KW - stars: individual (HD 3167)

KW - techniques: photometric

KW - techniques: spectroscopic

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DO - 10.3847/1538-3881/aa832d

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JO - Astronomical Journal

JF - Astronomical Journal

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ER -

Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

Abstract

Keywords

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Radial velocities for the HD 3167 system

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Three's Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

Abstract

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Datasets

Radial velocities for the HD 3167 system

Cite this