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Characterization of the Atmosphere of the Hot Jupiter HAT-P-32Ab and the M-dwarf Companion HAT-P-32B

Zhao, Ming and O'Rourke, Joseph G. and Wright, Jason T. and Knutson, Heather A. and Burrows, Adam and Fortney, Jonathan and Ngo, Henry and Fulton, Benjamin J. and Baranec, Christoph and Riddle, Reed and Law, Nicholas M. and Muirhead, Philip S. and Hinkley, Sasha and Showman, Adam P. and Curtis, Jason and Burruss, Rick (2014) Characterization of the Atmosphere of the Hot Jupiter HAT-P-32Ab and the M-dwarf Companion HAT-P-32B. Astrophysical Journal, 796 (2). Art. No. 115. ISSN 0004-637X.

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We report secondary eclipse photometry of the hot Jupiter HAT-P-32Ab, taken with Hale/Wide-field Infra-Red Camera (WIRC) in H and K_S bands and with Spitzer/IRAC at 3.6 and 4.5 μm. We carried out adaptive optics imaging of the planet host star HAT-P-32A and its companion HAT-P-32B in the near-IR and the visible. We clearly resolve the two stars from each other and find a separation of 2."923 ± 0."004 and a position angle 110.º64 ± 0.º12. We measure the flux ratios of the binary in g'r'i'z' and H and K_S bands, and determine T_(eff)= 3565 ± 82 K for the companion star, corresponding to an M1.5 dwarf. We use PHOENIX stellar atmosphere models to correct the dilution of the secondary eclipse depths of the hot Jupiter due to the presence of the M1.5 companion. We also improve the secondary eclipse photometry by accounting for the non-classical, flux-dependent nonlinearity of the WIRC IR detector in the H band. We measure planet-to-star flux ratios of 0.090% ± 0.033%, 0.178% ± 0.057%, 0.364% ± 0.016%, and 0.438% ± 0.020% in the H, K_S , 3.6 and 4.5 μm bands, respectively. We compare these with planetary atmospheric models, and find they prefer an atmosphere with a temperature inversion and inefficient heat redistribution. However, we also find that the data are equally well described by a blackbody model for the planet with T_p = 2042 ± 50 K. Finally, we measure a secondary eclipse timing offset of 0.3 ± 1.3 minutes from the predicted mid-eclipse time, which constrains e = 0.0072^(+0.0700)_(-0.0064) when combined with radial velocity data and is more consistent with a circular orbit.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Zhao, Ming0000-0002-4258-9517
O'Rourke, Joseph G.0000-0002-1180-996X
Wright, Jason T.0000-0001-6160-5888
Knutson, Heather A.0000-0002-0822-3095
Burrows, Adam0000-0002-3099-5024
Fortney, Jonathan0000-0002-9843-4354
Ngo, Henry0000-0001-5172-4859
Fulton, Benjamin J.0000-0003-3504-5316
Baranec, Christoph0000-0002-1917-9157
Riddle, Reed0000-0002-0387-370X
Law, Nicholas M.0000-0001-9380-6457
Muirhead, Philip S.0000-0002-0638-8822
Hinkley, Sasha0000-0001-8074-2562
Additional Information:© 2014 American Astronomical Society. Received 2014 August 15, accepted for publication 2014 October 2. Published 2014 November 13. We thank the anonymous referee for valuable comments for the paper. We thank the Palomar staff for their help with the observations. M.Z. is supported by funding from NASA Origins of Solar Systems grant NNX14AD22G and the Center for Exoplanets and Habitable Worlds at the Pennsylvania State University. 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. J.G.O. receives support from the National Science Foundation’s Graduate Research Fellowship Program. H.N. acknowledges funding support from the Natural Science and Engineering Research Council of Canada. A.B. acknowledges support in part under NASA HST grants HST-GO-12181.04-A, HST-GO-12314.03-A, HST-GO-12473.06-A, and HST-GO-12550.02, and JPL/Spitzer Agreements 1417122, 1348668, 1371432, 1377197, and 1439064. S.H. acknowledges support from the NASA Sagan Fellowship at California Institute of Technology. C.B. acknowledges support from the Alfred P. Sloan Foundation. The Palomar Hale 200 inch telescope is operated by Caltech and the Jet Propulsion Laboratory. The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, by the National Science Foundation under grant Nos. AST-0906060, AST-0960343, and AST-1207891, by a grant from the Mt. Cuba Astronomical Foundation and by a gift from Samuel Oschin. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at Facilities : Hale (WIRC), Spitzer (IRAC), PO:1.5m (Robo-AO), Keck:II (NIRC2
Funding AgencyGrant Number
Pennsylvania State UniversityUNSPECIFIED
Eberly College of ScienceUNSPECIFIED
Pennsylvania Space Grant ConsortiumUNSPECIFIED
NSF Graduate Research FellowshipUNSPECIFIED
Natural Science and Engineering Research Council of Canada (NSERC) UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Mt. Cuba Astronomical FoundationUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:binaries: general; infrared: planetary systems; planetary systems; stars: individual (HAT-P-32A, HAT-P-32B); techniques: high angular resolution; techniques: photometric
Record Number:CaltechAUTHORS:20141209-122039768
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Official Citation:Characterization of the Atmosphere of the Hot Jupiter HAT-P-32Ab and the M-dwarf Companion HAT-P-32B Ming Zhao et al. 2014 ApJ 796 115
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:52503
Deposited By: Ruth Sustaita
Deposited On:09 Dec 2014 22:40
Last Modified:06 Oct 2017 17:15

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