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Detection of Planetary Emission from TrES-2 using Spitzer/IRAC

Published online by Cambridge University Press:  01 May 2008

Francis T. O'Donovan ,
David Charbonneau ,
Joseph Harrington ,
Sara Seager ,
Drake Deming  and
Heather A. Knutson
Francis T. O'Donovan
Affiliation:
NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA email: francis.odonovan@nasa.gov, leo.d.deming@nasa.gov California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA
David Charbonneau
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA email: dcharbonneau@cfa.harvard.edu, hknutson@cfa.harvard.edu
Joseph Harrington
Affiliation:
Department of Physics, University of Central Florida, 4000 Central Florida Blvd., Orlando, FL 32816, USA email: jh@physics.ucf.edu
Sara Seager
Affiliation:
Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Ave., Cambridge, MA 02139, USA email: seager@mit.edu
Drake Deming
Affiliation:
NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA email: francis.odonovan@nasa.gov, leo.d.deming@nasa.gov
Heather A. Knutson
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA email: dcharbonneau@cfa.harvard.edu, hknutson@cfa.harvard.edu
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Abstract

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We present here results from observations of TrES-2 made using the Infrared Array Camera on the Spitzer Space Telescope. We monitored this transiting system during two secondary eclipses, when the planetary emission is blocked by the star. The resulting decrease in flux is 0.135 ± 0.036%, 0.245 ± 0.027%, 0.162 ± 0.064%, and 0.295 ± 0.066%, at 3.6-μm, 4.5-μm, 5.8-μm, and 8.0-μm, respectively. We find evidence for a temperature inversion in the atmosphere of TrES-2, which is predicted by Fortney and collaborators based on the proposed importance of TiO and VO opacities for this highly irradiated gas giant. We also find the time of the center of the eclipse to be consistent with predictions from transit timing observations of TrES-2. 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 of the large planetary radius.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S253: Transiting Planets , May 2008 , pp. 536 - 539
Copyright
Copyright © International Astronomical Union 2009

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