We compare the observed planet-to-star contrast of HD 189733 (large red points) in 56 wavelengths with a prediction based on a blackbody planet, i.e., isothermal atmosphere (solid black line). The broadband secondary eclipse depths measured by Charbonneau et al. (2008; black circles with error bars), Knutson et al. (2012), and Agol et al. (2010; black circles with no error bars at 3.6, 4.5, and 8 μm, respectively) using Spitzer IRAC and MIPS are also plotted. The Agol et al. (2010) measurement at 8 μm represents an average of six separate eclipse depth measurements. The size of the uncertainties of the Agol et al. (2010) and Knutson et al. (2012) results is indicated in the upper left for clarity. We show the band integrated contrasts predicted for a blackbody planet for the IRS data (blue stars) and the IRAC and MIPS bandpasses (green stars). The black dotted lines indicate the transmission functions of Spitzer IRAC and MIPS. We indicate the effective temperature of the planet assuming an isothermal atmosphere in the upper left, with uncertainties derived from the χ² distribution and based only on the spectroscopic data points. For this fit, the minimum . This value does not include the photometric points. The only degree of freedom here is the planetary temperature.