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Supernovae arise from progenitor stars occupying the upper end of the initialmass function. Their extreme brightness allows individual massive stars to bedetected at cosmic distances, lending supernovae great potential as tracers ofthe upper end of the IMF and its evolution. Exploiting this potential requiresprogress in many areas of supernova science. These include understanding theprogenitor masses that produce various types of supernovae and accuratelycharacterizing the supernova outburst and the environment in which it wasproduced. I present some preliminary work identifying the environmentalconditions that produce the most luminous supernovae, believed to arise fromstars with masses greater than 100 M_sun. I illustrate that the presence ofthese extreme supernovae in small star-forming dwarfs can be used to test ourunderstanding of the upper end of the IMF.

Measuring the Upper End of the Initial Mass Function with Supernovae