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KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Transiting the V = 8 Subgiant HD 93396

Pepper, Joshua and Mawet, Dimitri and Bottom, Michael and Fulton, Benjamin J. and Howard, Andrew W. (2017) KELT-11b: A Highly Inflated Sub-Saturn Exoplanet Transiting the V = 8 Subgiant HD 93396. Astronomical Journal, 153 (5). Art. No. 215. ISSN 0004-6256.

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We report the discovery of a transiting exoplanet, KELT-11b, orbiting the bright (V = 8.0) subgiant HD 93396. A global analysis of the system shows that the host star is an evolved subgiant star with T_(eff) = 5370±51 K, M∗ = 1.438^(+0.061)_(−0.052) M⊙, R∗ = 2.72^(+0.21)_(−0.17) R⊙, log g∗= 3.727^(+0.040)_(−0.046), and [Fe/H]= 0.180 ± 0.075. The planet is a low-mass gas giant in a P = 4.736529 ± 0.00006 day orbit, with M_P = 0.195 ± 0.018 M_J, R_P = 1.37^(+0.15)_(−0.12) R_J, ρ_P = 0.093^(+0.028)_(−0.024) g cm^(−3) , surface gravity log g_P = 2.407^(+0.080)_(−0.086), and equilibrium temperature T_(eq) = 1712^(+51)_(−46) K. KELT-11 is the brightest known transiting exoplanet host in the southern hemisphere by more than a magnitude, and is the 6th brightest transit host to date. The planet is one of the most inflated planets known, with an exceptionally large atmospheric scale height (2763 km), and an associated size of the expected atmospheric transmission signal of 5.6%. These attributes make the KELT-11 system a valuable target for follow-up and atmospheric characterization, and it promises to become one of the benchmark systems for the study of inflated exoplanets.

Item Type:Article
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URLURL TypeDescription Paper
Pepper, Joshua0000-0002-3827-8417
Mawet, Dimitri0000-0002-8895-4735
Bottom, Michael0000-0003-1341-5531
Fulton, Benjamin J.0000-0003-3504-5316
Howard, Andrew W.0000-0001-8638-0320
Additional Information:© 2017 The American Astronomical Society. Received 2016 July 6; revised 2017 March 3; accepted 2017 March 6; published 2017 April 18. Work by B.S.G. and D.J.S. was partially supported by NSF CAREER Grant AST-1056524. M.B. is supported by a NASA Space Technology Research Fellowship. J.P. would like to thank Stephen Faulkner and Katheryn Kirkwood for help during a difficult time. D.W.L acknowledges partial support from the Kepler Extended Mission under Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. D.B. acknowledges financial support from the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. T.B. was partially supported by funding from the Center for Exoplanets and Habitable Worlds. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. B.J.F. notes that this material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. Any opinion, findings, and conclusions or recommendations expressed in this material are those of the authors(s) and do not necessarily reflect the views of the National Science Foundation. This work has made use of NASAs Astrophysics Data System, the Extrasolar Planet Encyclopedia at (Schneider et al. 2011), the SIMBAD database operated at CDS, Strasbourg, France, and the VizieR catalog access tool, CDS, Strasbourg, France (Ochsenbein et al. 2000). Certain calculations in this paper were carried out on the Ruby cluster operated by the Ohio Supercomputer Center (Center 1987). MINERVA is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, University of Montana, and University of New South Wales. MINERVA is made possible by generous contributions from its collaborating institutions and Mt. Cuba Astronomical Foundation, The David & Lucile Packard Foundation, National Aeronautics and Space Administration (EPSCOR grant NNX13AM97A), and The Australian Research Council (LIEF grant LE140100050). This publication makes use of data products from the Widefield 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 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 paper makes use of data from the first public release of the WASP data (Butters et al. 2010) as provided by the WASP consortium and services at the NASA Exoplanet Archive (Akeson et al. 2013), which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program, the Exoplanet Orbit Database, and the Exoplanet Data Explorer at (Han et al. 2014).
Group:Infrared Processing and Analysis Center (IPAC), Astronomy Department
Funding AgencyGrant Number
NASA Space Technology Research FellowshipUNSPECIFIED
Swiss National Science Foundation (SNSF)UNSPECIFIED
Center for Exoplanets and Habitable WorldsUNSPECIFIED
Pennsylvania State UniversityUNSPECIFIED
Eberly College of ScienceUNSPECIFIED
Pennsylvania Space Grant ConsortiumUNSPECIFIED
NSF Graduate Research Fellowship2014184874
Subject Keywords:planetary systems – planets and satellites: detection – stars: individual (KELT-11) – techniques: photometric – techniques: radial velocities
Issue or Number:5
Record Number:CaltechAUTHORS:20160707-151707005
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Official Citation:Joshua Pepper et al 2017 AJ 153 215
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:68895
Deposited By: Joy Painter
Deposited On:08 Jul 2016 02:16
Last Modified:03 Oct 2019 10:17

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