Notes. Stellar masses have been obtained by fitting CIGALE (Boquien et al. 2019) SED models to available photometry from the literature (see appendix). B-band luminosities are from Svensson et al. (2010) based on literature photometry (see that paper for details). For GRB 031203, GRB 050826 and GRB 100316D we derived r₈₀, for GRB 020903 and GRB 050826 r₅₀ from FORS2, PanSTARRS and HST imaging used for the contours in Fig. 1, the remaining values are from Svensson et al. (2010) and Japelj et al. (2018). d_GRB is the distance of the GRB location from the spaxel containing the brightest Hα emission. SFRs are based on UV luminosities and taken from Michałowski et al. (2015) when not indicated differently, SSFRs are the SFR divided by the stellar mass, SFR densities are calculated as ΣSFR = SFR/. Metallicities are from the global host spectra using the N2 parameter and the Marino et al. (2013) calibration.

References. ^(a)Levesque et al. (2010b), ^(b)Thöne et al. (2007), ^(c)Levesque et al. (2010a), ^(d)Starling et al. (2012), ^(e)Svensson et al. (2010), ^(f)Wiersema et al. (2007), ^(g)Levesque et al. (2011), ^(h)Izzo et al. (2017), ⁽ⁱ⁾Japelj et al. (2018).