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We present an analysis of late-time Hubble Space Telescope Wide Field Camera3 and Wide Field Planetary Camera 2 observations of the site of the Type Ic SN2007gr in NGC 1058. The SN is barely recovered in the late-time WFPC2observations, while a possible detection in the later WFC3 data is debatable.These observations were used to conduct a multiwavelength study of thesurrounding stellar population. We fit spatial profiles to a nearby brightsource that was previously proposed to be a host cluster. We find that, ratherthan being an extended cluster, it is consistent with a single point-likeobject. Fitting stellar models to the observed spectral energy distribution ofthis source, we conclude it is A1-A3 Yellow Supergiant, possibly correspondingto a star with $M_{ZAMS} = 40M_{\odot}$. SN 2007gr is situated in a massivestar association, with diameter of $\approx 300\,\mathrm{pc}$. We present aBayesian scheme to determine the properties of the surrounding massive starpopulation, in conjunction with the Padova isochrones. We find that the stellarpopulation, as observed in either the WFC3 and WFPC2 observations, can be wellfit by two age distributions with mean ages: ~6.3 Myr and ~50 Myr. The stellarpopulation is clearly dominated by the younger age solution (by factors of 3.5and 5.7 from the WFPC2 and WFC3 observations, respectively), which correspondsto the lifetime of a star with $M_{ZAMS} \sim 30M_{\odot}$. This is strongevidence in favour of the hypothesis that SN 2007gr arose from a massiveprogenitor star, possibly capable of becoming a Wolf-Rayet star.

A high mass progenitor for the Type Ic Supernova 2007gr inferred from its environment