Fig. 8.
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Inner slope vs stellar mass for simulations running with the optimal FDM mass of 1.9 × 10−23 eV. In green appears the prediction of baryonic feedback simulations from Di Cintio et al. (2014), Tollet et al. (2016). We use a 1σ scatter of 0.3, matching closely with the results of Di Cintio et al. (2014), Tollet et al. (2016), while also adding an additional 2σ scatter band. The gray band represents a conservative scatter derived analytically for NFW profiles.
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