We observe two secondary eclipses of the strongly irradiated transiting planet WASP-33b , in the K _ { s } band at 2.15 \mu m , and one secondary eclipse each at 3.6 \mu m and 4.5 \mu m using Warm Spitzer . This planet orbits an A5V \delta -Scuti star that is known to exhibit low amplitude non-radial p-mode oscillations at about 0.1 % semi-amplitude . We detect stellar oscillations in all of our infrared eclipse data , and also in one night of observations at J-band ( 1.25 \mu m ) out of eclipse . The oscillation amplitude , in all infrared bands except K _ { s } , is about the same as in the optical . However , the stellar oscillations in K _ { s } band ( 2.15 \mu m ) have about twice the amplitude ( 0.2 % ) as seen in the optical , possibly because the Brackett- \gamma line falls in this bandpass . As regards the exoplanetary eclipse , we use our best-fit values for the eclipse depth , as well as the 0.9 \mu m eclipse observed by Smith et al . ( 51 ) , to explore possible states of the exoplanetary atmosphere , based on the method of Madhusudhan & Seager ( 40 ) . On this basis we find two possible states for the atmospheric structure of WASP-33b . One possibility is a non-inverted temperature structure in spite of the strong irradiance , but this model requires an enhanced carbon abundance ( C / O > 1 ) . The alternative model has solar composition , but an inverted temperature structure . Spectroscopy of the planet at secondary eclipse , using a spectral resolution that can resolve the water vapor band structure , should be able to break the degeneracy between these very different possible states of the exoplanetary atmosphere . However , both of those model atmospheres absorb nearly all of the stellar irradiance with minimal longitudinal re-distribution of energy , strengthening the hypothesis of Cowan & Agol ( 17 ) that the most strongly irradiated planets circulate energy poorly . Our measurement of the central phase of the eclipse yields e cos \omega = 0.0003 \pm 0.00013 , which we regard as being consistent with a circular orbit .