CCFs of the planetary emission spectrum for nights N1 (top panel) and N2 (bottom panel) as a function of the planetary orbital phase. The CCFs shown in these plots were computed using the Fe I spectral template, for which we claim the strongest detection (see Table 4). In each panel, the dashed white line marks where the planetary emission signal is expected according to the system parameters in Table 1. The emission trace is not obvious in this 2D plot and is only detected significantly in the K_p–υ_sys map, as shown in Fig. 3.