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tokens: different from those of normal SNe, and the study of the immediate environment of these events can provide important information on physical properties of their progenitors which so far have remained undetected. Fig. 1 Left panel : Pan-STARRS -band image of NGC 3191 with the PMAS (blue squares) and the MaNGA fields of view (red hexagon) superposed. Right panel : map of the H ii regions obtained with the code described in the text and applied to the PMAS cubes. The SLSN 2017egm position is marked with a red cross in both panels. The levels of the isophotes, from the outermost to the innermost, are 21.86, 21.11, 20.66, 20.22, and 19.91 mag/arcsec. Indeed, several studies of SLSN host galaxy samples have revealed significant differences in the properties of Type I and Type II hosts ( Leloudas et al. 2015 ; Perley et al. 2016 ; Lunnan et al. 2014 ; Schulze et al. 2016 ). Type I hosts are usually star-forming (SF) dwarf galaxies with low metallicities at the extreme end of the distribution in the Baldwin-Philips-Terlevich (BPT; Baldwin et al. 1981 ) diagram and likely even more extreme than gamma-ray burst (GRB) hosts (see e.g. Leloudas et al. 2015 ; Schulze et al. 2016 ; but see also Lunnan et al. 2014 ). In addition, they have been found in very young stellar populations, indicating that Type I SLSNe might be the first and most massive stars to end in a SN explosion after the onset of a new starburst episode in their galaxy or HII region ( Thöne et al. 2015 ). Type II hosts seem to be more metal rich and within the bulk of emission-line galaxies in the SDSS. At higher redshifts, Type I SLSN hosts evolve in line with the most star-forming galaxies towards higher-mass galaxies with higher absolute star formation rates (SFRs), but still seem to show a metallicity cut-off at 0.4 solar and a tendency towards low-mass hosts ( Schulze et al. 2016 ). In this paper, we present integral field unit (IFU) spectroscopic data of NGC 3191, the host galaxy of SN 2017egm, a Type I SLSN discovered by the Gaia satellite ( Delgado et al. 2017 ) on May 23, 2017. Detailed analysis of its early optical spectra revealed its Type I SLSN nature ( Dong et al. 2017 ; Nicholl et al. 2017 ). The SLSN reached its optical maximum on June 20, 2017, with an absolute magnitude of mag. As pointed out in Nicholl et al. (2017) , Bose et al. (2017) , and Chen et al. (2017b) , the host seems to be the first Type I host with super-solar metallicity. In this work, we analyse the properties of different regions in the host galaxy, and in the SLSN location, providing a more detailed analysis of the metallicity and the star formation rate distributions around the SLSN environment and several other H ii regions. Resolved spectral modelling across the host galaxy gives us important clues to the different underlying stellar populations, their ages, and their metallicities, allowing us a more detailed insight into this apparently very peculiar SLSN-I environment. 2. Observations We observed the