Degeneracy between thermal emission and reflected light for WASP-43b (Stevenson et al. 2014, 2017). The 1σ constraints from two published eclipse depths are shown. When ﹩{A}_{g}=0﹩, only thermal emission contributes to the eclipse depth. As A_g is increased, the amount of thermal emission decreases and, consequently, so does T_day. Only two wavelengths are shown here for clarity, but the following trend holds: the Spitzer IRAC eclipse depth lines never touch the horizontal axis for physically possible values of geometric albedo, meaning Spitzer measurements require thermal emission regardless of the value of A_g. For the HST/WFC3 measurements, the eclipse depths can be attributed solely to reflected light if the geometric albedo is ∼40%. It may not be safe to ignore reflected light in the HST/WFC3 1.1–1.7 μm bandpass.