The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog
Author:
Hill Michelle L.ORCID, Kane Stephen R.ORCID, Dalba Paul A.ORCID, MacDougall MasonORCID, Fetherolf TaraORCID, Li ZhexingORCID, Pidhorodetska DariaORCID, Batalha Natalie M.ORCID, Crossfield Ian J. M., Dressing CourtneyORCID, Fulton BenjaminORCID, Howard Andrew W.ORCID, Huber DanielORCID, Isaacson HowardORCID, Petigura Erik A.ORCID, Robertson PaulORCID, Weiss Lauren M.ORCID, Behmard AidaORCID, Beard CoreyORCID, Chontos AshleyORCID, Dai FeiORCID, Giacalone StevenORCID, Hirsch Lea A.ORCID, Holcomb RaeORCID, Lubin JackORCID, Mayo Andrew W.ORCID, Močnik TeoORCID, Murphy Joseph M. AkanaORCID, Polanski Alex S.ORCID, Rosenthal Lee J.ORCID, Rubenzahl Ryan A.ORCID, Scarsdale NicholasORCID, Turtelboom Emma V.ORCID, Van Zandt JudahORCID, Bieryla AllysonORCID, Ciardi David R.ORCID, Eastman Jason D.ORCID, Falk Ben, Hesse Katharine M.ORCID, Latham David W.ORCID, Livingston JohnORCID, Matson Rachel A.ORCID, Matthews ElisabethORCID, Ricker George R.ORCID, Rudat Alexander, Schlieder Joshua E.ORCID, Seager S.ORCID, Winn Joshua N.ORCID
Abstract
Abstract
The Transiting Exoplanet Survey Satellite (TESS) continues to increase dramatically the number of known transiting exoplanets, and is optimal for monitoring bright stars amenable to radial velocity (RV) and atmospheric follow-up observations. TOI-1386 is a solar-type (G5V) star that was detected via TESS photometry to exhibit transit signatures in three sectors with a period of 25.84 days. We conducted follow-up RV observations using Keck/High Resolution Echelle Spectrometer (HIRES) as part of the TESS–Keck Survey, collecting 64 RV measurements of TOI-1386 with the HIRES spectrograph over 2.5 yr. Our combined fit of the TOI-1386 photometry and RV data confirm the planetary nature of the detected TESS signal, and provide a mass and radius for planet b of 0.148 ± 0.019 M
J and 0.540 ± 0.017 R
J, respectively, marking TOI-1386 b as a warm sub-Saturn planet. Our RV data further reveal an additional outer companion, TOI-1386 c, with an estimated orbital period of 227.6 days and a minimum mass of 0.309 ± 0.038 M
J. The dynamical modeling of the system shows that the measured system architecture is long-term stable, although there may be substantial eccentricity oscillations of the inner planet due to the dynamical influence of the outer planet.
Publisher
American Astronomical Society
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