Even after the discovery of the first few afterglows of short-duration GRBs, it was apparent that they reside in a much broader range of galaxies than their long-duration cousins.  With reasonable sample sizes now in hand, we have learned that short GRBs can explode in star-forming galaxies, elliptical galaxies, and even on some occasions far away from any potential host (making identification quite challenging).  This directly indicates that their progenitors span a wide range of ages, potentially up to several Gyr.  Because stellar mass is split approximately evenly between early- and late-type galaxies at z < 1, a population that exclusively traced stellar mass would be expected to have a roughly even split in host galaxy type.  The fact that more short-duration GRBs occur in late-type galaxies (Figure 15) indicates that there is some correlation with ongoing star formation for short-duration GRBs.  However, the limits on the typical progenitor ages derived from this mix indicate a broad range, much larger than observed for long-duration GRBs.