  The 11 Mpc H-alpha and Ultraviolet Galaxy (11HUGS) Survey traces the star
formation activity of nearby galaxies. In addition within this volume the
detection completeness of core-collapse supernovae (CCSNe) is high therefore by
comparing these observed stellar births and deaths we can make a sensitive test
of our understanding of how stars live and die. In this paper, we use the
results of the Binary Population and Spectral Synthesis (BPASS) code to
simulate the 11HUGS galaxies H-alpha and far-ultraviolet (FUV) star formation
rate indicators (SFRIs) and simultaneously match the core-collapse supernova
(CCSN) rate. We find that stellar population including interacting binary stars
makes little difference to the total CCSN rate but increases the H-alpha and
FUV fluxes for a constant number of stars being formed. In addition they
significantly increase the predicted rate of type Ibc supernovae (SNe) relative
to type II SNe to the level observed in the 11HUGS galaxies. We also find that
instead of assuming a constant star formation history (SFH) for the galaxies
our best fitting models have a star formation rate (SFR) that peaked more than
3 Myrs ago.
