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Recent observations suggest that global properties of the host galaxies forlong-duration gamma-ray bursts (GRBs) are particularly well-suited for creatingthe massive star progenitors of these GRBs. Motivated by the hypothesis thatmassive young star clusters located in metal-poor, low-metallicity galaxies area natural birthsite for GRB progenitors, we present a comparison study of theISM properties along the sightline toward the super star cluster, NGC1705-1,and those in distant GRB hosts. Using the same set of metal transitions in theUV and applying known ISM structures in NGC1705, we find that NGC1705-1resembles distant GRB host galaxies in its high neutral gas column, lowmolecular gas fraction, low metallicity, alpha-element enhancement,and low dustdepletion. The lack of molecular gas is due to the enhanced UV radiation fieldin the starburst environment, consistent with the expectations for GRBprogenitors. In addition, the known presence of dense neutral gas clouds atr<500 pc from NGC1705-1 provides a natural reservoir of C^+, Si^+, and Fe^+ions that may be subsequently excited by the afterglow UV radiation field toproduce excited lines commonly seen in GRB host ISM. We further argue that theapparent offset in the velocity profiles of low- and high-ionizationtransitions from absorption-line observations alone already offers importantclues for related starburst episodes in GRB host galaxies. Our study shows thata statistical comparison between the ISM around star clusters and high-redshiftGRB progenitors is important for identifying the key physical parameters thatfacilitate the formation of GRBs.

Super Star Cluster NGC1705-1: A Local Analogue to the Birthsite of Long-duration Gamma-ray Bursts