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|Title:||SOPHIE velocimetry of Kepler transit candidates. XV. KOI-614b, KOI-206b, and KOI-680b: a massive warm Jupiter orbiting a G0 metallic dwarf and two highly inflated planets with a distant companion around evolved F-type stars||Authors:||Almenara, J. M.
Diaz, R. F.
Barros, S. C. C.
BONOMO, ALDO STEFANO
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||575||First Page:||A71||Abstract:||We report the validation and characterization of three new transiting exoplanets using SOPHIE radial velocities: KOI-614b, KOI-206b, and KOI-680b. KOI-614b has a mass of 2.86 ± 0.35 M<SUB>Jup</SUB> and a radius of 1.13 <SUP>+0.26</SUP><SUB>-0.18</SUB> R<SUB>Jup</SUB>, and it orbits a G0, metallic ([ Fe/H ] = 0.35 ± 0.15) dwarf in 12.9 days. Its mass and radius are familiar and compatible with standard planetary evolution models, so it is one of the few known transiting planets in this mass range to have an orbital period over ten days. With an equilibrium temperature of T<SUB>eq</SUB> = 1000 ± 45 K, this places KOI-614b at the transition between what is usually referred to as "hot" and "warm" Jupiters. KOI-206b has a mass of 2.82 ± 0.52 M<SUB>Jup</SUB> and a radius of 1.45 ± 0.16 R<SUB>Jup</SUB>, and it orbits a slightly evolved F7-type star in a 5.3-day orbit. It is a massive inflated hot Jupiter that is particularly challenging for planetary models because it requires unusually large amounts of additional dissipated energy in the planet. On the other hand, KOI-680b has a much lower mass of 0.84 ± 0.15 M<SUB>Jup</SUB> and requires less extra-dissipation to explain its uncommonly large radius of 1.99 ± 0.18 R<SUB>Jup</SUB>. It is one of the biggest transiting planets characterized so far, and it orbits a subgiant F9-star well on its way to the red giant stage, with an orbital period of 8.6 days. With host stars of masses of 1.46 ± 0.17 M<SUB>☉</SUB> and 1.54 ± 0.09 M<SUB>☉</SUB>, respectively, KOI-206b, and KOI-680b are interesting objects for theories of formation and survival of short-period planets around stars more massive than the Sun. For those two targets, we also find signs of a possible distant additional companion in the system. <P />Based on observations made with SOPHIE on the 1.93-m telescope at the Observatoire de Haute-Provence (CNRS), France.Figures 11-14 are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201424291/olm">http://www.aanda.org</A>||Acknowledgments:||This paper includes data collected with SOPHIE and ESPaDOnS and by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. We thank the technical team at the Observatoire de Haute-Provence for their support with the SOPHIE instrument and the 1.93-m telescope and, in particular, for the essential work of the night assistants. Financial support for the SOPHIE observations from the Programme National de Planétologie (PNP) of CNRS/INSU, France is gratefully acknowledged. We also acknowledge support from the French National Research Agency (ANR-08- JCJC-0102-01). Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. The team at LAM acknowledges support by CNES grants 98761 (SCCB), 426808 (CD), and 251091 (JMA). A.S. acknowledge the support from the Euro- pean Research Council/European Community under the FP7 through Starting Grant agreement number 239953. A.S. is supported by the European Union under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, number 627202. A.S.B. acknowledges funding from the European Union Seventh Framework Program (FP7/2007-2013) under Grant agreement No. 313014 (ETAEARTH). Part of this research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. JMA acknowledges funding from the European Research Council under the ERC Grant Agreement No. 337591-ExTrA.||URI:||http://hdl.handle.net/20.500.12386/28688||URL:||https://www.aanda.org/articles/aa/full_html/2015/03/aa24291-14/aa24291-14.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201424291||Bibcode ADS:||2015A&A...575A..71A||Fulltext:||open|
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