Spatially resolved MaNGA observations of the host galaxy of
  superluminous supernova 2017egm
  Superluminous supernovae (SLSNe) are found predominantly in dwarf galaxies,
indicating that their progenitors have a low metallicity. However, the most
nearby SLSN to date, SN 2017egm, occurred in the spiral galaxy NGC 3191, which
has a relatively high stellar mass and correspondingly high metallicity. In
this paper, we present detailed analysis of the nearby environment of SN
2017egm using MaNGA IFU data, which provides spectral data on kiloparsec
scales. From the velocity map we find no evidence that SN 2017egm occurred
within some intervening satellite galaxy, and at the SN position most
metallicity diagnostics yield a solar and above solar metallicity (12 + log
(O/H) = 8.8-9.1). Additionally we measure a small H-alpha equivalent width (EW)
at the SN position of just 34 Angs, which is one of the lowest EWs measured at
any SLSN or Gamma-Ray Burst position, and indicative of the progenitor star
being comparatively old. We also compare the observed properties of NGC 3191
with other SLSN host galaxies. The solar-metallicity environment at the
position of SN 2017egm presents a challenge to our theoretical understanding,
and our spatially resolved spectral analysis provides further constraints on
the progenitors of SLSNe.
