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tokens: Ia cluster rates with redshift has been used to explain the distribution of Fe in the ICM, as well as the SN Ia delay time distribution and respective predictions for single- versus double-degenerate progenitors (Sharon et al. 2010 ; Barbary et al. 2012 ; Friedmann Maoz 2018 ). Looking forward, assuming that the majority of short GRBs are linked to BNS merger progenitors, the true fraction of short GRBs that occur in galaxy clusters may similarly play a role in r -process element enrichment of the ICM and intracluster light (ICL). In addition, the large physical offsets of cluster short GRBs from their most probable hosts, relative to those associated with field galaxies, is of interest in understanding their origins. A natural explanation for the occurrence of short GRBs at tens of kiloparsecs away from their host galaxies, but within galaxy clusters, are the large systemic velocities that BNS systems may experience (Zevin et al. 2019 ), coupled with the older stellar population in clusters that contribute to longer delay times. Galaxy cluster studies have also shown that the ICL and BCGs compose ≈30%–50% of the cluster stellar mass (Zhang et al. 2019 ). In particular, the origins of the ICL and ICM have been linked to the disruption of dwarf galaxies (Gregg West 1998 ) or the tidal stripping of outer material from more typical galaxy cluster members (Gallagher et al. 1972 ; DeMaio et al. 2015 , 2018 ). Since 30% of short GRBs occur in the halos of their host galaxies (Fong Berger 2013 ; Zevin et al. 2019 ), beyond a few effective radii, the locations of these short GRBs are situated amid prime material for stripping to contribute to the ICL and ICM. 6. Conclusions We have presented identification of the early-type, quiescent host galaxy of GRB 161104A and a detailed investigation of the large-scale galaxy cluster environment surrounding GRB 161104A. We have also presented new modeling of 20 additional short GRB host galaxies, as well as the identification of the large-scale environment of GRB 090515 as a galaxy cluster. We summarize with the following conclusions: 1. The putative host of GRB 161104A is an early-type, quiescent galaxy at z = 0.793 ± 0.003. By jointly fitting the host photometry and spectroscopy from Magellan with Prospector , we determine a stellar mass of M ≈ 1.6 × 10 10 M ⊙ , mass-weighted age of t m ≈ 2.12 Gyr, metallicity of , dust extinction A V ≈ 0.08, and ongoing SFR ≈ 0.099 M ⊙ yr −1 . 2. Using deep optical and NIR observations, we determine that the host of GRB 161104A and most of the galaxies surrounding the XRT position are at similar redshifts of z ∼ 0.8. We confirm their membership in a cluster at a median redshift of z = 0.79 using DES cluster catalogs. We also show that GRB 090515 resides in a cluster at z ∼ 0.4. This makes GRB 161104A the fifth short GRB associated with a cluster and the highest-redshift short GRB known to be associated with a galaxy cluster. 3. We model the broadband SEDs of 20 additional