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We have used Hubble/WFC3 and the G141 grism to measure the secondary eclipseof the transiting very hot Jupiter CoRoT-2b in the 1.1-1.7$\mu$m spectralregion. We find an eclipse depth averaged over this band equal to$395^{+69}_{-45}$ parts per million, equivalent to a blackbody temperature of$1788\pm18$K. We study and characterize several WFC3 instrumental effects,especially the "hook" phenomenon described by Deming et al. (2013). We use datafrom several transiting exoplanet systems to find a quantitative relationbetween the amplitude of the hook and the exposure level of a given pixel.Although the uncertainties in this relation are too large to allow us todevelop an empirical correction for our data, our study provides a useful guidefor optimizing exposure levels in future WFC3 observations. We derive theplanet's spectrum using a differential method. The planet-to-star contrastincreases to longer wavelength within the WFC3 bandpass, but without waterabsorption or emission to a $3\sigma$ limit of 85 ppm. The slope of the WFC3spectrum is significantly less than the slope of the best-fit blackbody. Wecompare all existing eclipse data for this planet to a blackbody spectrum, andto spectra from both solar abundance and carbon-rich (C/O=1) models. Ablackbody spectrum is an acceptable fit to the full dataset. Extra continuousopacity due to clouds or haze, and flattened temperature profiles, are strongcandidates to produce quasi-blackbody spectra, and to account for the amplitudeof the optical eclipses. Our results show ambiguous evidence for a temperatureinversion in this planet.

The Emergent 1.1-1.7 Micron Spectrum of the Exoplanet CoRoT-2b as Measured Using the Hubble Space Telescope