Stars as cosmic scales: measuring stellar mass with microlensed supernovae

Gravitational microlensing is a unique probe of the stellar content in strong lens galaxies. Flux ratio anomalies from gravitationally lensed supernovae (glSNe), just like lensed quasars, can be used to constrain the stellar mass fractions at the image positions. Type Ia supernovae are of particular interest as knowledge of the intrinsic source brightness helps constrain the amount of (de)magnification from the macromodel predictions that might be due to microlensing. In addition, the presence or absence of caustic crossings in the light curves of glSNe can be used to constrain the mass of the microlenses. We find that a sample of 50 well-modeled glSNe Ia systems with single epoch observations at peak intrinsic supernova luminosity should be able to constrain an average stellar mass-to-light ratio to within $\sim 15\%$. A set of systems with light curve level information providing the location (or absence) of caustic crossing events can also constrain the mass of the microlenses to within $\sim 50\%$. Much work is needed to make such a measurement in practice, but our results demonstrate the feasibility of microlensing to place constraints on astrophysical parameters related to the initial mass function of lensing galaxies without any prior assumptions on the stellar mass.