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L.J. Richardson (LASP, Univ. of Colorado, and GSFC), D. Deming (GSFC), G. Wiedemann (Univ. Observatory, Munich), C. Goukenleuque (NAS/NRC at GSFC), L.W. Esposito (LASP, Univ. of Colorado), J. Harrington (Cornell Univ.)
We discuss the status of our observational program to detect infrared radiation from the "transiting planet," HD209458b. Current models suggest that the planet could be as hot as 1400K, with a significant infrared output in spectral bands having minimum water vapor opacity. Our differential spectroscopic technique is designed to detect the subtle change in the 2-4 micron spectrum as the planet is blocked by the star during secondary eclipse. We have observed the system during three secondary eclipse events: two in July 2001 using ISAAC at the VLT (3.5-3.7 microns, R=3300) and one in September 2001 using the SpeX instrument at the IRTF (1.9-4.2 microns, R=1500). Analysis of these extensive data is in progress. Although direct detection of the planet is not guaranteed, initial examination of the data lead us to be optimistic concerning the utility of our differential spectroscopic approach.
This work is sponsored by NASA's Origins of Solar Systems Program and by a NASA GSRF Fellowhsip to L.J.R.