Training custom light curve models of SN Ia subpopulations selected according to host galaxy properties

• Published in: Monthly notices of the Royal Astronomical Society 2024-03, Vol.528 (3), p.4643-4656
• Main Authors: Taylor, G, Lidman, C, Popovic, B, Abbot, H J
• Format: Article
• Language: English
• Subjects: Adaptive sampling; Astronomical models; Cosmology; Dark energy; Galaxy distribution; Light curve; Luminosity; Pluto; Populations; Sky surveys (astronomy); Spectral energy distribution; Standardization; Stars & galaxies; Step functions
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stae293

ABSTRACT Type Ia supernova (SN Ia) cosmology analyses include a luminosity step function in their distance standardization process to account for an observed yet unexplained difference in the post-standardization luminosities of SNe Ia originating from different host galaxy populations [e.g. high-mass ($M \gtrsim 10^{10} \, {\rm M}_{\odot }$) versus low-mass galaxies]. We present a novel method for including host-mass correlations in the SALT3 (Spectral Adaptive Light curve Template 3) light curve model used for standardizing SN Ia distances. We split the SALT3 training sample according to host-mass, training independent models for the low- and high-host-mass samples. Our models indicate that there are different average Si ii spectral feature strengths between the two populations, and that the average spectral energy distribution of SNe from low-mass galaxies is bluer than the high-mass counterpart. We then use our trained models to perform an SN cosmology analysis on the 3-yr spectroscopically confirmed Dark Energy Survey SN sample, treating SNe from low- and high-mass host galaxies as separate populations throughout. We find that our mass-split models reduce the Hubble residual scatter in the sample, albeit at a low statistical significance. We do find a reduction in the mass-correlated luminosity step but conclude that this arises from the model-dependent re-definition of the fiducial SN absolute magnitude rather than the models themselves. Our results stress the importance of adopting a standard definition of the SN parameters (x0, x1, c) in order to extract the most value out of the light curve modelling tools that are currently available and to correctly interpret results that are fit with different models.