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We report secondary eclipse photometry of two hot Jupiters, WASP-48b andHAT-P-23b, at 3.6 and 4.5 um taken with the InfraRed Array Camera aboard theSpitzer Space Telescope during the warm Spitzer mission and in the H and Ksbands with the Wide Field IR Camera at the Palomar 200-inch Hale Telescope.WASP-48b and HAT-P-23b are Jupiter-mass and twice Jupiter-mass objects orbitingan old, slightly evolved F star and an early G dwarf star, respectively. In theH, Ks, 3.6 um, and 4.5 um bands, respectively, we measure secondary eclipsedepths of 0.047% +/- 0.016%, 0.109% +/- 0.027%, 0.176% +/- 0.013%, and 0.214%+/- 0.020% for WASP-48b. In the Ks, 3.6 um, and 4.5 um bands, respectively, wemeasure secondary eclipse depths of 0.234% +/- 0.046%, 0.248% +/- 0.019%, and0.309% +/- 0.026% for HAT-P-23b. For WASP-48b and HAT-P-23b, respectively, wemeasure delays of 2.6 +/- 3.9 minutes and 4.0 +/- 2.4 minutes relative to thepredicted times of secondary eclipse for circular orbits, placing 2-sigma upperlimits on |e cos(omega)| of 0.0053 and 0.0080, both of which are consistentwith circular orbits. The dayside emission spectra of these planets arewell-described by blackbodies with effective temperatures of 2158 +/- 100 K(WASP-48b) and 2154 +/- 90 K (HAT-P-23b), corresponding to moderaterecirculation in the zero albedo case. Our measured eclipse depths are alsoconsistent with one-dimensional radiative transfer models featuring varyingdegrees of recirculation and weak thermal inversions or no inversions at all.We discuss how the absence of strong temperature inversions on these planetsmay be related to the activity levels and metallicities of their host stars.

Warm Spitzer and Palomar Near-IR Secondary Eclipse Photometry of Two Hot Jupiters: WASP-48b and HAT-P-23b