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A Precise Estimate of the Radius of HD 149026b

Published online by Cambridge University Press:  01 May 2008

Philip Nutzman
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 email: pnutzman@cfa.harvard.edu
David Charbonneau
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 email: pnutzman@cfa.harvard.edu Alfred P. Sloan Research Fellow
Joshua N. Winn
Affiliation:
Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Heather A. Knutson
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 email: pnutzman@cfa.harvard.edu
Jonathan J. Fortney
Affiliation:
Department of Astronomy and Astrophysics, UCO/Lick Observatory, University of California, Santa Cruz, CA 95064
Matthew J. Holman
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 email: pnutzman@cfa.harvard.edu
Eric Agol
Affiliation:
Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195
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Abstract

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We present Spitzer 8 μm transit observations of the extrasolar planet system HD 149026b. At this wavelength, transit light curves are weakly affected by stellar limb-darkening, allowing for a simpler and more accurate determination of planetary parameters. We measure a planet-star radius ratio of Rp/R∗=0.05158±0.00077, and in combination with ground-based data and independent constraints on the stellar mass and radius, we derive an orbital inclination of i = 85°.4+0°.9−0°.8 and a planet radius of 0.755 ± 0.040 RJ. These measurements further support models in which the planet is greatly enriched in heavy elements.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2009

References

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