- Main
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, BJ;
- Batygin, Konstantin;
- Benneke, Björn;
- Brewer, John M;
- Charbonneau, David;
- Ciardi, David R;
- Cameron, Andrew Collier;
- Coughlin, Jeffrey L;
- Crossfield, Ian JM;
- 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 MS;
- 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
- et al.
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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