As in Fig. 6, but for the MagAcc cases (cold and warm; left and right groups, respectively). The mass in M_J and accretion rate in M_J yr⁻¹ are indicated in each subpanel. The spectra are for an observer looking into the accretion flow towards the base of the shock or more generally for radiation passing through only the layers closest to the planet and escaping (see Fig. 1). Possible rotation and inclination (between the observer and the accretion column) are not taken into account. The strong photospheric absorption (green) in some cases may not be realistic; see text.