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The dayside of HD 149026b is near the edge of detectability by the SpitzerSpace Telescope. We report on eleven secondary-eclipse events at 3.6, 4.5, 3 x5.8, 4 x 8.0, and 2 x 16 microns plus three primary-transit events at 8.0microns. The eclipse depths from jointly-fit models at each wavelength are0.040 +/- 0.003% at 3.6 microns, 0.034 +/- 0.006% at 4.5 microns, 0.044 +/-0.010% at 5.8 microns, 0.052 +/- 0.006% at 8.0 microns, and 0.085 +/- 0.032% at16 microns. Multiple observations at the longer wavelengths improvedeclipse-depth signal-to-noise ratios by up to a factor of two and improvedestimates of the planet-to-star radius ratio (Rp/Rs = 0.0518 +/- 0.0006). Wealso identify no significant deviations from a circular orbit and, using thismodel, report an improved period of 2.8758916 +/- 0.14 days.Chemical-equilibrium models find no indication of a temperature inversion inthe dayside atmosphere of HD 149026b. Our best-fit model favors large amountsof CO and CO2, moderate heat redistribution (f=0.5), and a strongly enhancedmetallicity. These analyses use BiLinearly-Interpolated Subpixel Sensitivity(BLISS) mapping, a new technique to model two position-dependent systematics(intrapixel variability and pixelation) by mapping the pixel surface at highresolution. BLISS mapping outperforms previous methods in both speed andgoodness of fit. We also present an orthogonalization technique forlinearly-correlated parameters that accelerates the convergence of Markovchains that employ the Metropolis random walk sampler. The electronicsupplement contains light-curve files and supplementary figures.

Transit and Eclipse Analyses of Exoplanet HD 149026b Using BLISS Mapping