Two Warm Super-Earths Transiting the Nearby M Dwarf TOI-2095
Author:
Quintana Elisa V.ORCID, Gilbert Emily A.ORCID, Barclay ThomasORCID, Silverstein Michele L.ORCID, Schlieder Joshua E.ORCID, Cloutier RyanORCID, Quinn Samuel N.ORCID, Rodriguez Joseph E.ORCID, Vanderburg AndrewORCID, Hord Benjamin J.ORCID, Louie Dana R.ORCID, Ostberg Colby, Kane Stephen R.ORCID, Hoffman KelseyORCID, Rowe Jason F.ORCID, Arney Giada N.ORCID, Saxena Prabal, Richardson Taran, Clement Matthew S.ORCID, Kartvedt Nicholas M., Adams Fred C.ORCID, Alfred Marcus, Berger TravisORCID, Bieryla AllysonORCID, Bonney PaulORCID, Boyd PatriciaORCID, Cadieux CharlesORCID, Caldwell DouglasORCID, Ciardi David R.ORCID, Charbonneau DavidORCID, Collins Karen A.ORCID, Colón Knicole D.ORCID, Conti Dennis M.ORCID, Di Sora Mario, Domagal-Goldman Shawn, Dotson JessieORCID, Fauchez ThomasORCID, Gonzales Erica J.ORCID, Günther Maximilian N.ORCID, Hedges ChristinaORCID, Isopi GiovanniORCID, Kohler Erika, Kopparapu RaviORCID, Kostov Veselin B., Larsen Jeffrey A., Lopez Eric, Mallia Franco, Mandell AviORCID, Mullally Susan E.ORCID, Paudel Rishi R.ORCID, Powell Brian P.ORCID, Ricker George R.ORCID, Safonov Boris S.ORCID, Schwarz Richard P.ORCID, Sefako Ramotholo, Stassun Keivan G.ORCID, Wilson Robert, Winn Joshua N.ORCID, Vanderspek Roland K.ORCID
Abstract
Abstract
We report the detection and validation of two planets orbiting TOI-2095 (TIC 235678745). The host star is a 3700 K M1V dwarf with a high proper motion. The star lies at a distance of 42 pc in a sparsely populated portion of the sky and is bright in the infrared (K = 9). With data from 24 sectors of observation during Cycles 2 and 4 of the Transiting Exoplanet Survey Satellite, TOI-2095 exhibits two sets of transits associated with super-Earth-sized planets. The planets have orbital periods of 17.7 days and 28.2 days and radii of 1.30 R
⊕ and 1.39 R
⊕, respectively. Archival data, preliminary follow-up observations, and vetting analyses support the planetary interpretation of the detected transit signals. The pair of planets have estimated equilibrium temperatures of approximately 400 K, with stellar insolations of 3.23 and 1.73 S
⊕, placing them in the Venus zone. The planets also lie in a radius regime signaling the transition between rock-dominated and volatile-rich compositions. They are thus prime targets for follow-up mass measurements to better understand the properties of warm, transition-radius planets. The relatively long orbital periods of these two planets provide crucial data that can help shed light on the processes that shape the composition of small planets orbiting M dwarfs.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
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