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ABSTRACT We use the BayeSN hierarchical probabilistic SED model to analyse the optical–NIR (BVriYJH) light curves of 86 Type Ia supernovae (SNe Ia) from the Carnegie Supernova Project to investigate the SN Ia host galaxy dust law distribution and correlations between SN Ia Hubble residuals and host mass. Our Bayesian analysis simultaneously constrains the mass step and dust RV population distribution by leveraging optical–NIR colour information. We demonstrate how a simplistic analysis where individual RV values are first estimated for each SN separately, and then the sample variance of these point estimates is computed, overestimates the RV population variance R². This bias is exacerbated when neglecting residual intrinsic colour variation beyond that due to light curve shape. Instead, Bayesian shrinkage estimates of σR are more accurate, with fully hierarchical analysis of the light curves being ideal. For the 75 SNe with low-to-moderate reddening (peak apparent B − V ≤ 0. 3), we estimate an RV distribution with population mean μR = 2. 59 ± 0. 14, and standard deviation σR = 0. 62 ± 0. 16. Splitting this subsample at the median host galaxy mass (1010. 57 M⊙) yields consistent estimated RV distributions between low- and high-mass galaxies, with μR = 2. 79 ± 0. 18, σR = 0. 42 ± 0. 24, and μR = 2. 35 ± 0. 27, σR = 0. 74 ± 0. 36, respectively. When estimating distances from the full optical–NIR light curves while marginalizing over various forms of the dust RV distribution, a mass step of ≳0. 06 mag persists in the Hubble residuals at the median host mass.
Thorp et al. (Thu,) studied this question.