  Some hydrogen poor superluminous supernovae (SLSNe) exhibit bumps in the
tails of their light-curves associated with hydrogen features in their late
time spectra. Here we use the explosion parameters of one such SLSN -- SN
2017gci -- to search the stellar models of the Binary Population And Spectral
Synthesis (BPASS) code for potential progenitors. We find good matches for a 30
$M_{\odot}$ progenitor star in a binary system and no matches from single star
models. Common envelope and mass transfer after the giant branch, combined with
increased mass loss from strong stellar winds immediately before death, allow
the progenitor to lose its hydrogen envelope decades before the explosion. This
results in a hydrogen poor SLSN and allows for delayed interaction of the
ejecta with the lost stellar material
