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KELT-24b: A 5M_J Planet on a 5.6 day Well-Aligned Orbit around the Young V=8.3 F-star HD 93148

Rodriguez, Joseph E. and Eastman, Jason D. and Zhou, George and Quinn, Samuel N. and Beatty, Thomas G. and Penev, Kaloyan and Johnson, Marshall C. and Cargile, Phillip A. and Latham, David W. and Bieryla, Allyson and Collins, Karen A. and Dressing, Courtney D. and Ciardi, David R. and Relles, Howard M. and Murawski, Gabriel and Nishiumi, Taku and Yonehara, Atsunori and Lund, Michael B. and Stevens, Daniel J. and Stassun, Keivan G. and Gaudi, B. Scott and Colón, Knicole D. and Pepper, Joshua and Narita, Norio and Awiphan, Supachai and Chuanraksasat, Pongpichit and Benni, Paul and Ishimaru, Ryo and Yoshida, Fumi and Zambelli, Roberto and Garrison, Lehman H. and Wilson, Maurice L. and Cornachione, Matthew A. and Wang, Sharon X. and Labadie-Bartz, Jonathan and Rodríguez, Romy and Siverd, Robert J. and Yao, Xinyu and Bayliss, Daniel and Berlind, Perry and Calkins, Michael L. and Christiansen, Jessie L. and Cohen, David H. and Conti, Dennis M. and Curtis, Ivan A. and Depoy, D. L. and Esquerdo, Gilbert A. and Evans, Phil and Feliz, Dax and Fulton, Benjamin J. and Gregorio, Joao and Holoien, Thomas W. S. and James, David J. and Jayasinghe, Tharindu and Jang-Condell, Hannah and Jensen, Eric L. N. and Johnson, John A. and Joner, Michael D. and Kielkopf, John F. and Kuhn, Rudolf B. and Manner, Mark and Marshall, Jennifer L. and McLeod, Kim K. and McCrady, Nate and Oberst, Thomas E. and Oelkers, Ryan J. and Penny, Matthew T. and Reed, Phillip A. and Sliski, David H. and Shappee, B. J. and Stephens, Denise C. and Stockdale, Chris and Tan, Thiam-Guan and Trueblood, Mark and Trueblood, Pat and Villanueva, Steven, Jr. and Wittenmyer, Robert A. and Wright, Jason T. (2019) KELT-24b: A 5M_J Planet on a 5.6 day Well-Aligned Orbit around the Young V=8.3 F-star HD 93148. Astronomical Journal, 158 (5). Art. No. 197. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20190619-104609263

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Abstract

We present the discovery of KELT-24 b, a massive hot Jupiter orbiting a bright (V=8.3 mag, K=7.2 mag) young F-star with a period of 5.6 days. The host star, KELT-24 (HD 93148), has a T_(eff) =6508±49 K, a mass of M∗ = 1.461^(+0.056)_(−0.060) M_⊙, radius of R∗ = 1.506±0.022 R_⊙, and an age of 0.77^(+0.61)_(−0.42) Gyr. Its planetary companion (KELT-24 b) has a radius of R_P = 1.272^(+0.021)_(−0.022) R_J, a mass of MP = 5.18^(+0.21)_(−0.22) M_J, and from Doppler tomographic observations, we find that the planet's orbit is well-aligned to its host star's projected spin axis (λ = 2.6^(+5.1)_(−3.6)). The young age estimated for KELT-24 suggests that it only recently started to evolve from the zero-age main sequence. KELT-24 is the brightest star known to host a transiting giant planet with a period between 5 and 10 days. Although the circularization timescale is much longer than the age of the system, we do not detect a large eccentricity or significant misalignment that is expected from dynamical migration. The brightness of its host star and its moderate surface gravity make KELT-24b an intriguing target for detailed atmospheric characterization through spectroscopic emission measurements since it would bridge the current literature results that have primarily focused on lower mass hot Jupiters and a few brown dwarfs.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ab4136DOIArticle
https://arxiv.org/abs/1906.03276arXivDiscussion Paper
ORCID:
AuthorORCID
Rodriguez, Joseph E.0000-0001-8812-0565
Ciardi, David R.0000-0002-5741-3047
Lund, Michael B.0000-0003-2527-1598
Christiansen, Jessie L.0000-0002-8035-4778
Fulton, Benjamin J.0000-0003-3504-5316
Villanueva, Steven, Jr.0000-0001-6213-8804
Additional Information:© 2019 The American Astronomical Society. Received 2019 June 7; revised 2019 August 9; accepted 2019 August 31; published 2019 October 23. We thank Laura Kreidberg, Andrew Vanderburg, and James Kirk for their valuable discussions and insight. J.E.R. was supported by the Harvard Future Faculty Leaders Postdoctoral fellowship. Work by G.Z. is provided by NASA through Hubble Fellowship grant HST-HF2-51402.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. K.G.S. acknowledges support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics. T.N and A.Y. are also grateful to Mizuki Isogai, Akira Arai, and Hideyo Kawakita for their technical support on observations at Koyama Astronomical Observatory. This work is partly supported by JSPS KAKENHI grant Numbers JP18H01265 and JP18H05439, and JST PRESTO grant No. JPMJPR1775. J.L.-B. acknowledges support from FAPESP (grant 2017/23731-1). K.P. acknowledges support from NASA grants 80NSSC18K1009 and NNX17AB94G. This work makes use of observations from the LCOGT network. This research has made use of SAO/NASA's Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCO network. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. MINERVA is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, and the University of Southern Queensland. 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), The Australian Research Council (LIEF grant LE140100050), and the National Science Foundation (grants 1516242 and 1608203). Any opinions, findings, and conclusions or recommendations expressed are those of the author and do not necessarily reflect the views of the National Science Foundation. Funding for MINERVA data-analysis software development is provided through a subaward under NASA award MT-13-EPSCoR-0011. 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. The ASAS-SN observations are used to help vet exoplanet candidates from KELT. ASAS-SN would like to thank Las Cumbres Observatory and its staff for their continued support. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grant AST-1515927, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Villum Fonden (Denmark). Facilities: FLWO 1.5 m (Tillinghast Reflector Echelle Spectrograph - , TRES); Kilodegree Extremely Little Telescope (KELT); MINiature Exoplanet Radial Velocity Array (MINERVA); Las Cumbres Observatory at Tenerife (LCO TFN); University of Louisville Manner Telescope (ULMT - , Mt. Lemmon); KeplerCam (FLWO 1.2m); Stacja Obserwacji Tranzytów Egzoplanet w Suwałkach (SOTES); CROW Observatory; Koyama Astronomical Observatory (KAO). - Software: EXOFASTv2 (Eastman et al. 2013; Eastman 2017), AstroImageJ (Collins et al. 2017), SPC (Buchhave et al. 2010).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Harvard UniversityUNSPECIFIED
NASA Hubble FellowshipHST-HF2-51402.001-A
NASANAS 5-26555
Vanderbilt UniversityUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP18H01265
Japan Society for the Promotion of Science (JSPS)JP18H05439
Japan Science and Technology AgencyJPMJPR1775
Fundação de Amparo à Pesquisa do Estado de Sao Paulo (FAPESP) 2017/23731-1
NASA80NSSC18K1009
NASANNX17AB94G
Gaia Multilateral AgreementUNSPECIFIED
Mt. Cuba Astronomical FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
NASANNX13AM97A
Australian Research CouncilLE140100050
NSFAST-1516242
NSFAST-1608203
NASAMT-13-EPSCoR-0011
Pennsylvania State UniversityUNSPECIFIED
Eberly College of ScienceUNSPECIFIED
Pennsylvania Space Grant ConsortiumUNSPECIFIED
Gordon and Betty Moore FoundationGBMF5490
NSFAST-1515927
Ohio State UniversityUNSPECIFIED
Chinese Academy of Sciences South America Center for Astronomy (CASSACA)UNSPECIFIED
Villum FondenUNSPECIFIED
Subject Keywords:Transit photometry; Exoplanet astronomy; Exoplanet detection methods; Radial velocity
Issue or Number:5
Classification Code:Unified Astronomy Thesaurus concepts: Transit photometry (1709); Exoplanet astronomy (486); Exoplanet detection methods (489); Radial velocity (1332)
Record Number:CaltechAUTHORS:20190619-104609263
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190619-104609263
Official Citation:Joseph E. Rodriguez et al 2019 AJ 158 197
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96560
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 Jun 2019 18:11
Last Modified:23 Oct 2019 23:25

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