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

Journal
Date Issued
2017
Author(s)
Christiansen, Jessie L.
•
Vanderburg, Andrew
•
Burt, Jennifer
•
Fulton, B. J.
•
Batygin, Konstantin
•
Benneke, Björn
•
Brewer, John M.
•
Charbonneau, David
•
Ciardi, David R.
•
Collier Cameron, Andrew
•
Coughlin, Jeffrey L.
•
Crossfield, Ian J. M.
•
Dressing, Courtney
•
Greene, Thomas P.
•
Howard, Andrew W.
•
Latham, David W.
•
•
Mortier, Annelies
•
Mullally, Fergal
•
Pepe, Francesco
•
Rice, Ken
•
Sinukoff, Evan
•
•
Thompson, Susan E.
•
Udry, Stéphane
•
Vogt, Steven S.
•
Barman, Travis S.
•
Batalha, Natasha E.
•
Bouchy, François
•
Buchhave, Lars A.
•
Butler, R. Paul
•
•
Dupuy, Trent J.
•
Ehrenreich, David
•
Fiorenzano, Aldo
•
Hansen, Brad M. S.
•
Henning, Thomas
•
Hirsch, Lea
•
Holden, Bradford P.
•
Isaacson, Howard T.
•
Johnson, John A.
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Knutson, Heather A.
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Kosiarek, Molly
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López-Morales, Mercedes
•
Lovis, Christophe
•
•
Mayor, Michel
•
•
Motalebi, Fatemeh
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Petigura, Erik
•
Phillips, David F.
•
Piotto, Giampaolo
•
Rogers, Leslie A.
•
Sasselov, Dimitar
•
Schlieder, Joshua E.
•
Ségransan, Damien
•
Watson, Christopher A.
•
Weiss, Lauren M.
DOI
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}\oplus for HD 3167 b, a hot super-Earth with a likely rocky composition ({ρ }b = {5.60}-1.43+2.15 g cm-3), and {9.80}-1.24+1.30 {M}\oplus for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement ({ρ }c = {1.97}-0.59+0.94 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}\oplus . 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.
Volume
154
Issue
3
Start page
122
Uri
Url
Issn Identifier
0004-6256
Ads BibCode
2017AJ....154..122C
Rights
open.access
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