Abstract: Kilonovae are ultraviolet, optical, and infrared transients powered by the radioactive decay of heavy elements following a neutron star merger. Observations of kilonovae, joint with gravitational wave detections, may offer strong constraints on Galactic r-process enrichment, among other astrophysical topics. Unfortunately, kilonova emission rapidly fades within days to weeks, requiring quick and efficient astronomical follow-up to best capture this dimming thermal glow. In this talk, I will describe the ability of numerous wide field-of-view instruments to detect kilonovae, quantifying the maximum redshift reach of each instrument. I consider a selection of current and upcoming instruments, including ZTF, DECam, and the Vera C. Rubin Observatory’s LSST. These detectability predictions are model-dependent, based on the Los Alamos National Laboratory grid of kilonova models which spans a wide range of anticipated kilonova ejecta parameters.