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We present full-orbit phase curve observations of the eccentric ($e\sim0.08$) transiting hot Jupiter WASP-14b obtained in the 3.6 and 4.5 $\mu$m bandsusing the \textit{Spitzer Space Telescope}. We use two different methods forremoving the intrapixel sensitivity effect and compare their efficacy indecoupling 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 andfind it to be $9\%\pm 1\%$ of the dayside flux, corresponding to a brightnesstemperature 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-dimensionalradiative transfer and three-dimensional general circulation models. We findthat WASP-14b's measured dayside emission is consistent with a model atmospherewith equilibrium chemistry and a moderate temperature inversion. These samemodels tend to over-predict the nightside emission at 3.6 $\mu$m, whileunder-predicting the nightside emission at 4.5 $\mu$m. We propose that thisdiscrepancy might be explained by an enhanced global C/O ratio. In addition, wefind that the phase curves of WASP-14b ($7.8 M_{\mathrm{Jup}}$) are consistentwith a much lower albedo than those of other Jovian mass planets with thermalphase curve measurements, suggesting that it may be emitting detectable heatfrom the deep atmosphere or interior processes.

3.6 and 4.5 $\mu$m Phase Curves of the Highly-Irradiated Eccentric Hot Jupiter WASP-14b