  We present a brief summary of observations of the transiting extrasolar
planet, HD 209458 b, designed to detect the secondary eclipse. We employ the
method of `occultation spectroscopy', which searches in combined light (star
and planet) for the disappearance and reappearance of weak infrared spectral
features due to the planet as it passes behind the star and reappears. We have
searched for a continuum peak near 2.2 micron (defined by CO and H2O absorption
bands), as predicted by some models of the planetary atmosphere to be
approximately 6E-4 of the stellar flux, but no such peak is detected at a level
of about 3E-4 of the stellar flux. Our results represent the strongest limits
on the infrared spectrum of the planet to date and carry significant
implications for understanding the planetary atmosphere.
