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|Title:||SOPHIE velocimetry of Kepler transit candidates. XVI. Tomographic measurement of the low obliquity of KOI-12b, a warm Jupiter transiting a fast rotator||Authors:||Bourrier, V.
Lecavelier des Etangs, A.
Almenara, J. M.
Barros, S. C. C.
BONOMO, ALDO STEFANO
Diaz, R. F.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||579||First Page:||A55||Abstract:||We present the detection and characterization of the transiting warm Jupiter KOI-12b, first identified with Kepler with an orbital period of 17.86 days. We combine the analysis of Kepler photometry with Doppler spectroscopy and line-profile tomography of time-series spectra obtained with the SOPHIE spectrograph to establish its planetary nature and derive its properties. To derive reliable estimates for the uncertainties on the tomographic model parameters, we devised an empirical method of calculating statistically independent error bars on the time-series spectra. KOI-12b has a radius of 1.43 ± 0.13 R<SUB>Jup</SUB> and a 3σ upper mass limit of 10 M<SUB>Jup</SUB>. It orbits a fast-rotating star (vsini<SUB>⋆</SUB> = 60.0 ± 0.9 km s<SUP>-1</SUP>) with mass and radius of 1.45 ± 0.09 M<SUB>☉</SUB> and 1.63 ± 0.15 R<SUB>☉</SUB>, located at 426 ± 40 pc from the Earth. Doppler tomography allowed higher precision on the obliquity to be reached by comparison with analysis of the Rossiter-McLaughlin radial velocity anomaly, and we find that KOI-12b lies on a prograde, slightly misaligned orbit with low sky-projected obliquity λ = 12.6<SUP>3.0</SUP><SUB>-2.9</SUB>°. The properties of this planetary system, with a 11.4 mag host star, make of KOI-12b a precious target for future atmospheric characterization. <P />Tables 2 and 4 are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201525750/olm">http://www.aanda.org</A>||Acknowledgments:||We would like to offer particular thanks to the referee for their in-depth reading and very constructive comments. This publication is based on observations collected with the NASA satellite Kepler and the SOPHIE spectrograph on the 1.93 m telescope at Observatoire de Haute-Provence (CNRS), France (programs 12A.PNP.MOUT, 13A.PNP.MOUT, and 14A.PNP.HEBR). The authors acknowledge the support of the French Agence Nationale de la Recherche (ANR), under program ANR-12-BS05-0012 “Exo-Atmos”. This work has also been supported by an award of the Fondation Simone et Cino Del Duca. 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. Bonomo acknowledges funding from the European Union Seventh Framework Program (FP7/2007-2013) under Grant agreement number 313014 (ETAEARTH). This research has made use of the Extrasolar Planets Encyclopaedia at exoplanet.eu as well as the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org||URI:||http://hdl.handle.net/20.500.12386/28682||URL:||https://www.aanda.org/articles/aa/full_html/2015/07/aa25750-15/aa25750-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201525750||Bibcode ADS:||2015A&A...579A..55B||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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