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While optical surveys regularly discover slow transients like supernovae ontheir own, the most common way to discover extragalactic fast transients,fading away in a few nights, is via follow-up observations of gamma-ray burstand gravitational-wave triggers. However, wide-field surveys have the potentialto also identify rapidly fading transients independently of such externaltriggers. The volumetric survey speed of the Zwicky Transient Facility (ZTF)makes it sensitive to faint and fast-fading objects as kilonovae, the opticalcounterparts to binary neutron stars and neutron star-black hole mergers, outto almost 200Mpc. We introduce an open-source software infrastructure, the ZTFREaltime Search and Triggering, ZTFReST, designed to identify kilonovae andfast optical transients in ZTF data. Using the ZTF alert stream combined withforced photometry, we have implemented automated candidate ranking based ontheir photometric evolution and fitting to kilonova models. Automatedtriggering of follow-up systems, such as Las Cumbres Observatory, has also beenimplemented. In 13 months of science validation, we found several extragalacticfast transients independent of any external trigger (though some counterpartswere identified later), including at least one supernova with post-shockcooling emission, two known afterglows with an associated gamma-ray burst, twoknown afterglows without any known gamma-ray counterpart, and three newfast-declining sources (ZTF20abtxwfx, ZTF20acozryr, and ZTF21aagwbjr) that arelikely associated with GRB200817A, GRB201103B, and GRB210204A. However, we havenot found any objects which appear to be kilonovae; therefore, we constrain therate of GW170817-like kilonovae to $R < 900$Gpc$^{-3}$yr$^{-1}$. A frameworksuch as ZTFReST could become a prime tool for kilonova and fast transientdiscovery with the Vera C. Rubin Observatory.

astrophysical journal/the astrophysical journal

Fast-transient Searches in Real Time with ZTFReST: Identification of  Three Optically-discovered Gamma-ray Burst Afterglows and New Constraints on  the Kilonova Rate