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3.6 and 4.5μm Phase Curves of the Highly Irradiated Eccentric Hot Jupiter WASP-14b

Wong, Ian and Knutson, Heather A. and Lewis, Nikole K. and Kataria, Tiffany and Burrows, Adam and Fortney, Jonathan J. and Schwartz, Joel and Agol, Eric and Cowan, Nicolas B. and Deming, Drake and Désert, Jean-Michel and Fulton, Benjamin J. and Howard, Andrew W. and Langton, Jonathan and Laughlin, Gregory and Showman, Adam P. and Todorov, Kamen (2015) 3.6 and 4.5μm Phase Curves of the Highly Irradiated Eccentric Hot Jupiter WASP-14b. Astrophysical Journal, 811 (2). Art. No. 122. ISSN 0004-637X.

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We present full-orbit phase curve observations of the eccentric (e ~ 0.08) transiting hot Jupiter WASP-14b obtained in the 3.6 and 4.5 μm bands using the Spitzer Space Telescope. We use two different methods for removing the intrapixel sensitivity effect and compare their efficacy in decoupling the instrumental noise. Our measured secondary eclipse depths of 0.1882% ± 0.0048% and 0.2247% ± 0.0086% at 3.6 and 4.5 μm, respectively, are both consistent with a blackbody temperature of 2402 ± 35 K. We place a 2σ upper limit on the nightside flux at 3.6 μm and find it to be 9% ± 1% of the dayside flux, corresponding to a brightness temperature of 1079 K. At 4.5 μm, the minimum planet flux is 30% ± 5% of the maximum flux, corresponding to a brightness temperature of 1380 ± 65 K. We compare our measured phase curves to the predictions of one-dimensional radiative transfer and three-dimensional general circulation models. We find that WASP-14b's measured dayside emission is consistent with a model atmosphere with equilibrium chemistry and a moderate temperature inversion. These same models tend to overpredict the nightside emission at 3.6 μm, while underpredicting the nightside emission at 4.5 μm. We propose that this discrepancy might be explained by an enhanced global C/O ratio. In addition, we find that the phase curves of WASP-14b (7.8 M_(Jup)) are consistent with a much lower albedo than those of other Jovian mass planets with thermal phase curve measurements, suggesting that it may be emitting detectable heat from the deep atmosphere or interior processes.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Wong, Ian0000-0001-9665-8429
Knutson, Heather A.0000-0002-0822-3095
Lewis, Nikole K.0000-0002-8507-1304
Kataria, Tiffany0000-0003-3759-9080
Burrows, Adam0000-0002-3099-5024
Fortney, Jonathan J.0000-0002-9843-4354
Agol, Eric0000-0002-0802-9145
Cowan, Nicolas B.0000-0001-6129-5699
Deming, Drake0000-0001-5727-4094
Désert, Jean-Michel0000-0002-0875-8401
Fulton, Benjamin J.0000-0003-3504-5316
Howard, Andrew W.0000-0001-8638-0320
Laughlin, Gregory0000-0002-3253-2621
Todorov, Kamen0000-0002-9276-8118
Additional Information:© 2015. The American Astronomical Society. Received 2015 May 11; accepted 2015 August 28; published 2015 September 28. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The authors wish to thank J. I. Moses, J. K. Teske, and T. T. Koskinen for many useful discussions during the preparation of this manuscript. The authors also thank an anonymous reviewer for constructive comments that helped to improve the manuscript.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Subject Keywords:binaries: eclipsing; planetary systems; stars: individual (WASP-14) ; techniques: photometric
Issue or Number:2
Record Number:CaltechAUTHORS:20151119-145042986
Persistent URL:
Official Citation:Ian Wong et al 2015 ApJ 811 122
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:62267
Deposited By: Ruth Sustaita
Deposited On:19 Nov 2015 23:15
Last Modified:09 Mar 2020 13:18

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