TY - JOUR
T1 - The Kepler-19 System
T2 - A Thick-envelope Super-Earth with Two Neptune-mass Companions Characterized Using Radial Velocities and Transit Timing Variations
AU - Malavolta, Luca
AU - Borsato, Luca
AU - Granata, Valentina
AU - Piotto, Giampaolo
AU - Lopez, Eric
AU - Vanderburg, Andrew
AU - Figueira, Pedro
AU - Mortier, Annelies
AU - Nascimbeni, Valerio
AU - Affer, Laura
AU - Bonomo, Aldo S.
AU - Bouchy, Francois
AU - Buchhave, Lars A.
AU - Charbonneau, David
AU - Cameron, Andrew Collier
AU - Cosentino, Rosario
AU - Dressing, Courtney D.
AU - Dumusque, Xavier
AU - Fiorenzano, Aldo F.M.
AU - Harutyunyan, Avet
AU - Haywood, Raphaëlle D.
AU - Johnson, John Asher
AU - Latham, David W.
AU - Lopez-Morales, Mercedes
AU - Lovis, Christophe
AU - Mayor, Michel
AU - Micela, Giusi
AU - Molinari, Emilio
AU - Motalebi, Fatemeh
AU - Pepe, Francesco
AU - Phillips, David F.
AU - Pollacco, Don
AU - Queloz, Didier
AU - Rice, Ken
AU - Sasselov, Dimitar
AU - Ségransan, Damien
AU - Sozzetti, Alessandro
AU - Udry, Stéphane
AU - Watson, Chris
N1 - Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved..
PY - 2017/5
Y1 - 2017/5
N2 - We report a detailed characterization of the Kepler-19 system. This star was previously known to host a transiting planet with a period of 9.29 days, a radius of 2.2 R ⊕, and an upper limit on the mass of 20 M ⊕. The presence of a second, non-transiting planet was inferred from the transit time variations (TTVs) of Kepler-19b over eight quarters of Kepler photometry, although neither the mass nor period could be determined. By combining new TTVs measurements from all the Kepler quarters and 91 high-precision radial velocities obtained with the HARPS-N spectrograph, using dynamical simulations we obtained a mass of 8.4 ±1.6 M ⊕ for Kepler-19b. From the same data, assuming system coplanarity, we determined an orbital period of 28.7 days and a mass of 13.1 ±2.7 M ⊕ for Kepler-19c and discovered a Neptune-like planet with a mass of 20.3 ±3.4 M ⊕ on a 63-day orbit. By comparing dynamical simulations with non-interacting Keplerian orbits, we concluded that neglecting interactions between planets may lead to systematic errors that can hamper the precision in the orbital parameters when the data set spans several years. With a density of 4.32 ±0.87 g cm-3 (0.78 ±0.16 ρ ⊕) Kepler-19b belongs to the group of planets with a rocky core and a significant fraction of volatiles, in opposition to low-density planets characterized only by transit time variations and an increasing number of rocky planets with Earth-like density. Kepler-19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.
AB - We report a detailed characterization of the Kepler-19 system. This star was previously known to host a transiting planet with a period of 9.29 days, a radius of 2.2 R ⊕, and an upper limit on the mass of 20 M ⊕. The presence of a second, non-transiting planet was inferred from the transit time variations (TTVs) of Kepler-19b over eight quarters of Kepler photometry, although neither the mass nor period could be determined. By combining new TTVs measurements from all the Kepler quarters and 91 high-precision radial velocities obtained with the HARPS-N spectrograph, using dynamical simulations we obtained a mass of 8.4 ±1.6 M ⊕ for Kepler-19b. From the same data, assuming system coplanarity, we determined an orbital period of 28.7 days and a mass of 13.1 ±2.7 M ⊕ for Kepler-19c and discovered a Neptune-like planet with a mass of 20.3 ±3.4 M ⊕ on a 63-day orbit. By comparing dynamical simulations with non-interacting Keplerian orbits, we concluded that neglecting interactions between planets may lead to systematic errors that can hamper the precision in the orbital parameters when the data set spans several years. With a density of 4.32 ±0.87 g cm-3 (0.78 ±0.16 ρ ⊕) Kepler-19b belongs to the group of planets with a rocky core and a significant fraction of volatiles, in opposition to low-density planets characterized only by transit time variations and an increasing number of rocky planets with Earth-like density. Kepler-19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.
KW - planetary systems
KW - planets and satellites: composition
KW - planets and satellites: dynamical evolution and stability
KW - stars: individual (Kepler-19)
KW - techniques: photometric
KW - techniques: radial velocities
UR - http://www.scopus.com/inward/record.url?scp=85019047549&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/aa6897
DO - 10.3847/1538-3881/aa6897
M3 - Article
AN - SCOPUS:85019047549
SN - 0004-6256
VL - 153
JO - Astronomical Journal
JF - Astronomical Journal
IS - 5
M1 - 224
ER -