A New 24 μm Phase Curve for υ Andromedae b

doi:10.1088/0004-637X/723/2/1436

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Ian J. M. Crossfield et al. 2010 ApJ 723 1436 doi:10.1088/0004-637X/723/2/1436

A NEW 24 μm PHASE CURVE FOR υ ANDROMEDAE b

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Ian J. M. Crossfield¹, Brad M. S. Hansen^1,2, Joseph Harrington³, James Y.-K. Cho⁴, Drake Deming⁵, Kristen Menou⁶ and Sara Seager⁷

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ianc@astro.ucla.edu hansen@astro.ucla.edu jh@physics.ucf.edu J.Cho@qmul.ac.uk Leo.D.Deming@nasa.gov kristen@astro.columbia.edu seager@mit.edu

¹ Department of Physics and Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA
² Institute of Geophysics and Planetary Physics, University of California Los Angeles, Los Angeles, CA 90095, USA
³ Planetary Sciences Group, Department of Physics, University of Central Florida, Orlando, FL 32816-2385, USA
⁴ School of Mathematical Sciences, Queen Mary, University of London, London E1 4NS, UK
⁵ Planetary Systems Branch Code 693, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
⁶ Department of Astronomy, Columbia University, New York, NY 10027, USA
⁷ Department of Earth, Atmospheric and Planetary Sciences, Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA

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Abstract References Cited By

We report the detection of 24 μm variations from the planet-hosting υ Andromedae system consistent with the orbital periodicity of the system's innermost planet, υ And b. We find a peak-to-valley phase curve amplitude of 0.00130 times the mean system flux. Using a simple model with two hemispheres of constant surface brightness and assuming a planetary radius of 1.3 R_J give a planetary temperature contrast of gsim 900 K and an orbital inclination of gsim 28°. We further report the largest phase offset yet observed for an extrasolar planet: the flux maximum occurs ~80° before phase 0.5. Such a large phase offset is difficult to reconcile with most current atmospheric circulation models. We improve on earlier observations of this system in several important ways: (1) observations of a flux calibrator star demonstrate the MIPS detector is stable to 10^–4 on long timescales, (2) we note that the background light varies systematically due to spacecraft operations, precluding use of this background as a flux calibrator (stellar flux measured above the background is not similarly affected), and (3) we calibrate for flux variability correlated with motion of the star on the MIPS detector. A reanalysis of our earlier observations of this system is consistent with our new result.

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A NEW 24 μm PHASE CURVE FOR υ ANDROMEDAE b

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