Deming, DrakeKnutson, HeatherAgol, EricDesert, Jean-MichelBurrows, AdamFortney, Jonathan J.Charbonneau, DavidLaughlin, GregoryLangton, JonathanShowman, Adam P.Lewis, Nikole K.2019-09-242011Deming, Drake, Heather Knutson, Eric Agol, Jean-Michel Desert, Adam Burrows, Jonathan J. Fortney, David Charbonneau, et al. 2010. “WARMSPITZERPHOTOMETRY OF THE TRANSITING EXOPLANETS CoRoT-1 AND CoRoT-2 AT SECONDARY ECLIPSE.” The Astrophysical Journal 726 (2): 95. https://doi.org/10.1088/0004-637x/726/2/95.0004-637X1538-4357http://nrs.harvard.edu/urn-3:HUL.InstRepos:41397438We measure secondary eclipses of the hot giant exoplanets CoRoT-1 at 3.6 and 4.5 mu m, and CoRoT-2 at 3.6 mu m, both using Warm Spitzer. We find that the Warm Spitzer mission is working very well for exoplanet science. For consistency of our analysis we also re-analyze archival cryogenic Spitzer data for secondary eclipses of CoRoT-2 at 4.5 and 8 mu m. We compare the total data for both planets, including optical eclipse measurements by the CoRoT mission, and ground-based eclipse measurements at 2 mu m, to existing models. Both planets exhibit stronger eclipses at 4.5 than at 3.6 mu m, which is often indicative of an atmospheric temperature inversion. The spectrum of CoRoT-1 is best reproduced by a 2460 K blackbody, due either to a high altitude layer that strongly absorbs stellar irradiance, or an isothermal region in the planetary atmosphere. The spectrum of CoRoT-2 is unusual because the 8 mu m contrast is anomalously low. Non-inverted atmospheres could potentially produce the CoRoT-2 spectrum if the planet exhibits line emission from CO at 4.5 mu m, caused by tidal-induced mass loss. However, the viability of that hypothesis is questionable because the emitting region cannot be more than about 30% larger than the planet's transit radius, based on the ingress and egress times at eclipse. An alternative possibility to account for the spectrum of CoRoT-2 is an additional opacity source that acts strongly at wavelengths less than 5 mu m, heating the upper atmosphere while allowing the deeper atmosphere seen at 8 mu m to remain cooler. We obtain a similar result as Gillon et al. for the phase of the secondary eclipse of CoRoT-2, implying an eccentric orbit with e cos(omega) = -0.0030 +/- 0.0004.en-USJournal Article2019-09-2410.1088/0004-637X/726/2/95