8-Micron Photometry of the "Hot Saturn" HD 149026b During Its Secondary Eclipse

Details 8-Micron Photometry of the "Hot Saturn" HD 149026b During Its Secondary Eclipse 8-Micron Photometry of the "Hot Saturn" HD 149026b During Its Secondary Eclipse

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop..254h&link_type=abstract

Spitzer Proposal ID #254

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Scientific paper

We will measure the flux of the newly-discovered extrasolar planet HD149026b in the 8-micron IRAC bandpass during its secondary eclipse. The observation lasts 6 hours. HD 149026b is a transiting "hot Saturn" planet that was announced on 1 July 2005 (Sato et al. 2005). The planet is unusual for its small size and high density. At 0.725 Rj and 0.36 Mj, it is 1.7 times as dense as Saturn. Models predict that it must have a heavy-element core of 67-78 Earth masses, and that the core should extend more than half the distance to the surface, not unlike Neptune's and Uranus's cores. This unusual composition could result in substantially different atmospheric minor constituents, albedo, chemistry, and dynamics from those of any other planet. It thus bears immediate study, both for its own sake and to provide the basic flux numbers needed to plan follow-on studies in GO Cycles 3, 4, and 5. We have demonstrated that we can analyze and publish such data very quickly: manuscript submission for our Spitzer MIPS-24 detection of HD 209458b during its secondary eclipse (Deming et al. 2005b) took under two months from the receipt of data, without the benefit of pre-existing similar analyses, such as we now have. There had previously been no direct detection of light from an extrasolar planet. These pioneering measurements of HD 149026b's fluxes will give us two fluxes temperatures and possibly an H2O band depth. These will strongly constrain the many competing radiative, chemical, and dynamical models that are certain to appear in short order.

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