Fig. 11
Absolute change in HRs due to peculiar velocity correction for SNe Ia that belong to clusters as a function of supernova parameters (X1, C; triangles), host properties (local specific SFR (yr−1kpc−2), stellarmass (M⊙), morphological type, RS residuals [
]; circles; Childress et al. 2013; Brown et al. 2014; Rigault et al. 2018), relative SN position inside the cluster and cluster mass M200 (M⊙); squares. The colorbar shows the corresponding local specific SFR.
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