have similar masses to those of regular Type Ic-bl SNe, thus largely eliminating the possibility that the observed LGRB metallicity bias is somehow a byproduct of a difference in the initial stellar mass functions. [@Modjaz2008] showed that Ic-bl SNe with associated LGRBs are observed to occur in host galaxies with much lower metallicities than the hosts of Type Ic-bl SNe without associated LGRBs or the bulk of the star-forming galaxies in the SDSS. More recently [@Modjaz2019] has shown that Ic-bl in the local universe typically have low host metallicities essentially identical to LGRBs. (The [-@Modjaz2008] sample had a large number of SN found in directed surveys of nearby massive galaxies that may have produced this biased result.) However, beginning with LGRB 051022 [@conference_proceedings], some LGRBs were found to be located in host galaxies with a high metallicity (near-solar and above) but this accounted for only a small fraction of the LGRB population. The dramatic metallicity difference between both the star-formation weighted SDSS and non-engine driven SNe verses LGRB samples (including normal Type Ic, c.f. [@Modjaz2019] suggests a metallicity dependent step in either the formation of the gamma-ray jet or in its ability to escape the progenitor which has either burned 