We present full-orbit phase curve observations of the eccentric ( e \sim 0.08 ) transiting hot Jupiter WASP-14b obtained in the 3.6 and 4.5 \mu m bands using the Spitzer Space Telescope .
We use two different methods for removing the intrapixel sensitivity effect and compare their efficacy in decoupling the instrumental noise .
Our measured secondary eclipse depths of 0.1882 \% \pm 0.0048 \% and 0.2247 \% \pm 0.0086 \% at 3.6 and 4.5 \mu m , respectively , are both consistent with a blackbody temperature of 2402 \pm 35 K. We place a 2 \sigma upper limit on the nightside flux at 3.6 \mu m and find it to be 9 \% \pm 1 \% of the dayside flux , corresponding to a brightness temperature of 1079 K. At 4.5 \mu m , the minimum planet flux is 30 \% \pm 5 \% of the maximum flux , corresponding to a brightness temperature of 1380 \pm 65 K. We compare our measured phase curves to the predictions of one-dimensional radiative transfer and three-dimensional general circulation models .
We find that WASP-14b ’ s measured dayside emission is consistent with a model atmosphere with equilibrium chemistry and a moderate temperature inversion .
These same models tend to over-predict the nightside emission at 3.6 \mu m , while under-predicting the nightside emission at 4.5 \mu m. We propose that this discrepancy might be explained by an enhanced global C/O ratio .
In addition , we find that the phase curves of WASP-14b ( 7.8 ~ { } M _ { \mathrm { Jup } } ) are consistent with a much lower albedo than those of other Jovian mass planets with thermal phase curve measurements , suggesting that it may be emitting detectable heat from the deep atmosphere or interior processes .