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 journalArticle

20 Citations (Scopus)

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.

Original languageEnglish (US)
Article number122
JournalAstronomical Journal
Volume154
Issue number3
DOIs
StatePublished - Sep 1 2017

Fingerprint

planets
planet
inclination
atmospheric composition
Neptune (planet)
Neptune
thermal emission
transit
radial velocity
complement
oscillation
spectroscopy
geometry
stars
oscillations
configurations

Keywords

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

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Christiansen, J. L., Vanderburg, A., Burt, J., Fulton, B. J., Batygin, K., Benneke, B., ... 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

Three's Company : An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets. / Christiansen, Jessie L.; Vanderburg, Andrew; Burt, Jennifer; Fulton, B. J.; Batygin, Konstantin; Benneke, Björn; Brewer, John M.; Charbonneau, David; Ciardi, David R.; Cameron, Andrew Collier; Coughlin, Jeffrey L.; Crossfield, Ian J.M.; Dressing, Courtney; Greene, Thomas P.; Howard, Andrew W.; Latham, David W.; Molinari, Emilio; Mortier, Annelies; Mullally, Fergal; Pepe, Francesco; Rice, Ken; Sinukoff, Evan; Sozzetti, Alessandro; Thompson, Susan E.; Udry, Stéphane; Vogt, Steven S.; Barman, Travis S; Batalha, Natasha E.; Bouchy, François; Buchhave, Lars A.; Butler, R. Paul; Cosentino, Rosario; Dupuy, Trent J.; Ehrenreich, David; Fiorenzano, Aldo; Hansen, Brad M.S.; Henning, Thomas; Hirsch, Lea; Holden, Bradford P.; Isaacson, Howard T.; Johnson, John A.; Knutson, Heather A.; Kosiarek, Molly; López-Morales, Mercedes; Lovis, Christophe; Malavolta, Luca; Mayor, Michel; Micela, Giuseppina; Motalebi, Fatemeh; Petigura, Erik; Phillips, David F.; Piotto, Giampaolo; Rogers, Leslie A.; Sasselov, Dimitar; Schlieder, Joshua E.; Ségransan, Damien; Watson, Christopher A.; Weiss, Lauren M.

In: Astronomical Journal, Vol. 154, No. 3, 122, 01.09.2017.

Research output: Contribution to journalArticle

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
Christiansen, Jessie L. ; Vanderburg, Andrew ; Burt, Jennifer ; Fulton, B. J. ; Batygin, Konstantin ; Benneke, Björn ; Brewer, John M. ; Charbonneau, David ; Ciardi, David R. ; Cameron, Andrew Collier ; Coughlin, Jeffrey L. ; Crossfield, Ian J.M. ; Dressing, Courtney ; Greene, Thomas P. ; Howard, Andrew W. ; Latham, David W. ; Molinari, Emilio ; Mortier, Annelies ; Mullally, Fergal ; Pepe, Francesco ; Rice, Ken ; Sinukoff, Evan ; Sozzetti, Alessandro ; Thompson, Susan E. ; Udry, Stéphane ; Vogt, Steven S. ; Barman, Travis S ; Batalha, Natasha E. ; Bouchy, François ; Buchhave, Lars A. ; Butler, R. Paul ; Cosentino, Rosario ; Dupuy, Trent J. ; Ehrenreich, David ; Fiorenzano, Aldo ; Hansen, Brad M.S. ; Henning, Thomas ; Hirsch, Lea ; Holden, Bradford P. ; Isaacson, Howard T. ; Johnson, John A. ; Knutson, Heather A. ; Kosiarek, Molly ; López-Morales, Mercedes ; Lovis, Christophe ; Malavolta, Luca ; Mayor, Michel ; Micela, Giuseppina ; Motalebi, Fatemeh ; Petigura, Erik ; Phillips, David F. ; Piotto, Giampaolo ; Rogers, Leslie A. ; Sasselov, Dimitar ; Schlieder, Joshua E. ; Ségransan, Damien ; Watson, Christopher A. ; Weiss, Lauren M. / Three's Company : An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets. In: Astronomical Journal. 2017 ; Vol. 154, No. 3.
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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.",
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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.

PY - 2017/9/1

Y1 - 2017/9/1

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.

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KW - stars: individual (HD 3167)

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