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The collapsar model predicts that the progenitors of Gamma-ray Bursts (GRBs)are metal poor in Fe group elements. The existence of low metallicity stellarpopulations could manifest itself through special characteristics of theimmediate environment of the GRB site in the host galaxy. We analyse the strongemission lines from the sub-luminous host galaxy of GRB 980425, which showedthe first connection with a supernova explosion (SN 1998bw). The host has asufficient size to allow detailed resolved spectroscopy of individual HIIregions and to look for regions with special properties close to the the GRBsite. Using integral field spectroscopy with VIMOS we cover most of the highsurface brightness part of the host including the HII region where thesupernova and GRB occurred. The star formation rate, reddening, equivalentwidth and stellar mass in the GRB region is similar to other HII regions in thehost. Extreme values arise in the only region that shows emission lines fromWolf-Rayet stars; a region that lies 800 pc in projection from the GRB site.Strong emission line diagnostics of all HII regions imply oxygen abundancesbetween 0.3 and 0.8 solar with the lowest values arising in the WR and GRBregions. Comparing the measured emission line ratios for a sample of lowredshift GRB hosts to theoretical models and to observations of field galaxies,we find that GRBs arise in a range of metallicity environments while theregions are consistently very young. The similar line ratios of GRB hostscompared to the WR region can arise in spatially unresolved galaxies withbright HII regions near the GRB location. (Abridged)

IFU observations of the GRB 980425/SN 1998bw host galaxy: emission line ratios in GRB regions