Modeled planetary emission spectra (left panels) and the corresponding T–p profiles with volume mixing ratios (VMRs, right panels). We used different T–p profiles for the two species and computed the VMRs assuming equilibrium chemistry with solar elemental abundances. The upper and the lower panels refer to TiO and Fe, respectively. The CARMENES wavelength range is shaded in pink; the HARPS-N wavelength range is shaded in green; the ranges overlap. The spectral lines are stronger in the CARMENES range when compared to HARPS-N. A different scaling is applied to the planet-to-star flux contrast ratio on the y-axis of the spectra. The spectral lines of Fe are stronger when compared with the TiO model spectrum.