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Detection of Planetary Emission from the Exoplanet Tres-2 Using Spitzer/IRAC

O'Donovan, Francis T. and Charbonneau, David and Harrington, Joseph and Madhusudhan, N. and Seager, Sara and Deming, Drake and Knutson, Heather A. (2010) Detection of Planetary Emission from the Exoplanet Tres-2 Using Spitzer/IRAC. Astrophysical Journal, 710 (2). pp. 1551-1556. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20100225-165652168

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Abstract

We present here the results of our observations of TrES-2 using the Infrared Array Camera on Spitzer. We monitored this transiting system during two secondary eclipses, when the planetary emission is blocked by the star. The resulting decrease in flux is 0.127% ± 0.021%, 0.230% ± 0.024%, 0.199% ± 0.054%, and 0.359% ± 0.060% at 3.6 μm, 4.5 μm, 5.8 μm, and 8.0 μm, respectively. We show that three of these flux contrasts are well fit by a blackbody spectrum with T_(eff) = 1500 K, as well as by a more detailed model spectrum of a planetary atmosphere. The observed planet-to-star flux ratios in all four IRAC channels can be explained by models with and without a thermal inversion in the atmosphere of TrES-2, although with different atmospheric chemistry. Based on the assumption of thermochemical equilibrium, the chemical composition of the inversion model seems more plausible, making it a more favorable scenario. TrES-2 also falls in the category of highly irradiated planets which have been theoretically predicted to exhibit thermal inversions. However, more observations at infrared and visible wavelengths would be needed to confirm a thermal inversion in this system. Furthermore, we find that the times of the secondary eclipses are consistent with previously published times of transit and the expectation from a circular orbit. This implies that TrES-2 most likely has a circular orbit, and thus does not obtain additional thermal energy from tidal dissipation of a non-zero orbital eccentricity, a proposed explanation for the large radius of this planet.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1088/0004-637X/710/2/1551DOIArticle
https://arxiv.org/abs/0909.3073arXivDiscussion Paper
ORCID:
AuthorORCID
O'Donovan, Francis T.0000-0002-4858-6106
Charbonneau, David0000-0002-9003-484X
Madhusudhan, N.0000-0002-4869-000X
Seager, Sara0000-0002-6892-6948
Deming, Drake0000-0001-5727-4094
Knutson, Heather A.0000-0002-0822-3095
Additional Information:© 2010 American Astronomical Society. Print publication: Issue 2 (2010 February 20); received 2009 September 16; accepted for publication 2010 January 2; published 2010 February 1. 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 the National Aeronautics and Space Administration (NASA). This research was supported in part by NASA under grant NNG05GJ29G (issued through the Origins of Solar Systems Program) and also by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center (administered by Oak Ridge Associated Universities through a contract with NASA). Facilities: Spitzer (IRAC)
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANNG05GJ29G
NASA Postdoctoral ProgramUNSPECIFIED
Subject Keywords:eclipses; infrared: stars; planetary systems; stars: individual (GSC 03549-02811); techniques: photometric
Record Number:CaltechAUTHORS:20100225-165652168
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100225-165652168
Official Citation:Detection of Planetary Emission from the Exoplanet Tres-2 Using Spitzer/IRAC Francis T. O'Donovan, David Charbonneau, Joseph Harrington, N. Madhusudhan, Sara Seager, Drake Deming, and Heather A. Knutson 2010 ApJ 710 1551-1556 doi: 10.1088/0004-637X/710/2/1551
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17603
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:26 Feb 2010 19:37
Last Modified:21 May 2019 20:05

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