tokens: ( 2015 ). 2.1. Data Data for these studies were collected by reviewing published papers and searching both exoplanet.eu (Schneider et al. 2011 ) and exoplanets.org (Han et al. 2014 ). We start with the six planets in Table 2 of Schwartz Cowan ( 2015 ) that have thermal eclipses and phase amplitudes (at wavelengths longward of 0.8 μ m): HD 149026b, HD 189733b, HD 209458b, WASP-12b, WASP-18b, and WASP-43b. Then we add WASP-14b (Wong et al. 2015 ), HAT-P-7b, and WASP-19b (Wong et al. 2016 ) to our sample. We also incorporate new data from Zhou et al. ( 2015 ), Evans et al. ( 2015 ), and Line et al. ( 2016 ). We collect first-order phase offsets (Sections 2.2 and 2.2.1 ) from Knutson et al. ( 2009a , 2009b ) and Wong et al. ( 2015 , 2016 ). Knutson et al. ( 2009a ) concluded the offset they found was not statistically significant, so we use their largest uncertainty (72° ± 61°). Phase offsets through second order come from Cowan et al. ( 2012 ), Knutson et al. ( 2012 ), Maxted et al. ( 2013 ), Zellem et al. ( 2014 ), and Stevenson et al. ( 2014c , 2017 ). However, the second-order components in Zellem et al. ( 2014 ) were found to be unnecessary, and those at 4.5 micron in Cowan et al. ( 2012 ) are disputed, so we use neither in our fits. Also, Cowan et al. ( 2012 ) reported two sets of fit parameters for WASP-12b based on different models for detector systematics 7 7 Stevenson et al. ( 2014a ) fit eclipse depths for WASP-12b but not phase parameters, so we do not use their values in our analysis. —we use parameters from their preferred polynomial model but test the other scenario in Section 3.1 . 8 8 WASP-12 has binary companion stars that affect photometry of the system (Bechter et al. 2014 ). We use dilution factors from Stevenson et al. ( 2014b ) to correct observations of WASP-12b when appropriate. All nine planets in our study have non-zero offsets in at least one waveband. 2.2. Model We take an energy balance approach to interpreting thermal phase variations (e.g., Cowan Agol 2011b ): we compare the radiation going into and coming out from a planet to infer bulk energetics of that planet’s atmosphere. For our study, we use the energy balance model described in Section 3.1 of Schwartz Cowan ( 2015 ), which accounts for uncertainties in system parameters, as well as reflected light contamination, meridional heat transport, and other sources of uncertainty. Those authors treated stars as blackbodies; we estimate better stellar brightness temperatures for each observation by using BT-NextGen spectra (Allard et al. 2012 ). Then we use our compiled data to calculate the relative intensity of planets and their host stars at each observed wavelength. In Cowan Agol ( 2011b ) and Schwartz Cowan ( 2015 ), this nightside intensity ratio, ψ n ( λ ), is defined aswhere δ ecl is the eclipse depth, δ var is the peak-to-trough phase amplitude of the full light curve, and δ tr is the transit depth. This is exact only when an observation has no phase offset
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