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Here we present an integral-field study of the massive, high-metallicityspiral NGC 3191, the host of SN 2017egm, the closest SLSN Type I to date. Weuse data from PMAS/CAHA and the public MaNGA survey to shed light on theproperties of the SLSN site and the origin of star-formation in thisnon-starburst spiral galaxy. We map the physical properties different\ion{H}{II} regions throughout the galaxy and characterize their stellarpopulations using the STARLIGHT fitting code. Kinematical information allows tostudy a possible interaction with its neighbouring galaxy as the origin ofrecent star formation activity which could have caused the SLSN. NGC 3191 showsintense star-formation in the western part with three large SF regions of lowmetallicity. The central regions of the host have a higher metallicity, lowerspecific star-formation rate and lower ionization. Modeling the stellarpopulations gives a different picture: The SLSN region has two dominant stellarpopulations with different ages, the youngest one with an age of 2-10 Myr andlower metallicity, likely the population from which the SN progenitororiginated. Emission line kinematics of NGC 3191 show indications ofinteraction with its neighbour MCG+08-19-017 at $\sim$45 kpc, which might beresponsible for the recent starburst. In fact, this galaxy pair has in totalhosted 4 SNe, 1988B (Type Ia), SN 2003ds (Type Ic in MCG+08-19-017), PTF10bgl(SLSN-Type II) and 2017egm, underlying the enhanced SF in both galaxies due tointeraction. Our study shows that one has to be careful interpreting globalhost and even gas properties without looking at the stellar population historyof the region. SLSNe seem to still be consistent with massive stars ($>$ 20M$_\odot$) requiring low ($< 0.6Z_{\odot}$) metallicity and those environmentscan also occur in massive, late-type galaxies but not necessarily starbursts.

The host of the Type I SLSN 2017egm: A young, sub-solar metallicity environment in a massive spiral galaxy