Comparison with the atmospheric model of GJ 1214b from Miller-Ricci & Fortney (2010). The left panel shows the dayside temperature–pressure profile at ﹩{T}_{\mathrm{eff}}=660﹩ K. The temperatures in the infrared photosphere (﹩\sim {10}^{-2}﹩–1 bar) match very well. We also reproduce the temperatures in the deep atmosphere when an artificial opacity of ﹩6\times {10}^{-4}﹩ cm² g⁻¹ is inserted into the visible wavelengths (dashed curve). We can mimic the convective tail by adding internal heat flux, shown here for ﹩{T}_{\mathrm{intern}}=60﹩ K (cyan). The right panel depicts the corresponding planetary emission for three models of the left panel, together with a blackbody emission at the same effective temperature for comparison. The spectrum of Miller-Ricci & Fortney (2010) shows more pronounced features, but overall has the same magnitude. The HELIOS runs are similar because the main temperature difference lies below the emitting photosphere.