Fig. 1
Stellar input spectra, scaled to reach a surface temperature of 288.15 K, of the modelled planet and binned to a resolving power of 200. AD Leo and GJ 644 are taken from the VPL website (Segura et al. 2003), TRAPPIST-1 from O’Malley-James & Kaltenegger (2017), the other M-dwarf spectra from the MUSCLES database (France et al. 2016), and the solar spectrum from Gueymard (2004). Stars labelled with an asterisk are active M dwarfs. Top panel: UV and IR spectra up to 3 μm with linear axes. Bottom panel: UV spectra with logarithmic axes.
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