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We compare the chemical abundances at the sites of 12 nearby (z <0.14) TypeIc supernovae (SN Ic) that showed broad lines, but had no observed Gamma-RayBurst (GRB), with the chemical abundances in 5 nearby (z < 0.25) galaxies atthe sites of GRB where broad-lined SN Ic were seen after the fireball hadfaded. It has previously been noted that GRB hosts are low in luminosity andlow in their metal abundances. If low metallicity is sufficient to force theevolution of massive stars to end their lives as GRB with an accompanyingbroad-lined SN Ic, then we would expect higher metal abundances for thebroad-lined SN Ic that have no detected GRB. This is what we observe, and thistrend is independent of the choice of metallicity calibration we adopt, and themode of SN survey that found the broad-lined SN. A unique feature of thisanalysis is that we present new spectra of the host galaxies and analyze allthe measurements of both samples in the same set of ways, using the galaxyemission-line measurements corrected for extinction and stellar absorption, viaindependent metallicity diagnostics of Kewley & Dopita (2002), of McGaugh(1991) and of Pettini & Pagel (2004). In our small sample, the boundary betweengalaxies that have GRB accompanying their broad-lined SN Ic and those that havebroad-lined SN Ic without a GRB lies at an oxygen abundance of 12+log(O/H)_KD02~ 8.5, which corresponds to 0.2-0.6 Z_sun depending on the adopted metallicityscale and solar abundance value. Even when we limit the comparison to SN Icthat were found in untargeted supernova surveys, the environment of everybroad-lined SN Ic that had no GRB is more metal rich than the site of anybroad-lined SN Ic where a GRB was detected.

MEASURED METALLICITIES AT THE SITES OF NEARBY BROAD-LINED TYPE Ic SUPERNOVAE AND IMPLICATIONS FOR THE SUPERNOVAE GAMMA-RAY BURST CONNECTION