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We present H and Ks-band photometry bracketing the secondary eclipse of thehot Jupiter TrES-3b using the Wide-field Infrared Camera on theCanada-France-Hawaii Telescope. We detect the secondary eclipse of TrES-3b witha depth of 0.133+/-0.017% in Ks-band (8-sigma) - a result in sharp contrast tothe eclipse depth reported by de Mooij & Snellen. We do not detect its thermalemission in H-band, but place a 3-sigma limit on the depth of the secondaryeclipse in this band of 0.051%. A secondary eclipse of this depth in Ksrequires very efficient day-to-nightside redistribution of heat and nearlyisotropic reradiation, conclusion that is in agreement with longer wavelength,mid-infrared Spitzer observations. Our 3-sigma upper-limit on the depth of ourH-band secondary eclipse also argues for very efficient redistribution of heatand suggests that the atmospheric layer probed by these observations may bewell homogenized. However, our H-band upper limit is so constraining that itsuggests the possibility of a temperature inversion at depth, or an absorbingmolecule, such as methane, that further depresses the emitted flux at thiswavelength. The combination of our near-infrared measurements and thoseobtained with Spitzer suggest that TrES-3b displays a near isothermal daysideatmospheric temperature structure, whose spectrum is well approximated by ablackbody. We emphasize that our strict H-band limit is in stark disagreementwith the best-fit atmospheric model that results from longer wavelengthobservations only, thus highlighting the importance of near-infraredobservations at multiple wavelengths in addition to those returned by Spitzerin the mid-infrared to facilitate a comprehensive understanding of the energybudgets of transiting exoplanets.

Near-Infrared Thermal Emission from TrES-3b: A Ks-band detection and an H-band upper limit on the depth of the secondary eclipse