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The effect of progenitor metallicity on Type Ia Supernovae (SNe Ia) hasimportant cosmological implications due to the need for these standardizablecandles to be compared across large spans of cosmic time in which theprogenitor stars might have different properties. Theoretical models have cometo different conclusions as to the wavelength range impacted by metallicitydifferences, leading to differing interpretations of the growing sample of UVobservations. Recent work has claimed a correlation between the mid-UV flux ofSNe Ia measured from Swift grism spectra and the gas-phase metallicitiesmeasured for their host galaxies. Here we examine UV photometry for the sameobjects. We find no significant correlations between the UV-optical colors (orUV/optical count rate ratios) of the SNe Ia and the host galaxy properties ofmass or metallicity. The lack of a significant correlation with host galaxymetallicity implies another physical difference other than progenitormetallicity dominates the UV flux differences. We are no longer limited by alack of UV observations. Rather, understanding the existing observationsrequires improved theoretical models and a larger parameter space of physicaldifferences.

A Photometric Analysis of the Relationship Between Type Ia Supernova UV Flux and Host Galaxy Metallicity