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On 2019 August 14, the Advanced LIGO and Virgo interferometers detected thehigh-significance gravitational wave (GW) signal S190814bv. The GW dataindicated that the event resulted from a neutron star--black hole (NSBH)merger, or potentially a low-mass binary black hole merger. Due to the lowfalse alarm rate and the precise localization (23 deg$^2$ at 90\%), S190814bvpresented the community with the best opportunity yet to directly observe anoptical/near-infrared counterpart to a NSBH merger. To search for potentialcounterparts, the GROWTH collaboration performed real-time image subtraction on6 nights of public Dark Energy Camera (DECam) images acquired in the threeweeks following the merger, covering $>$98\% of the localization probability.Using a worldwide network of follow-up facilities, we systematically undertookspectroscopy and imaging of optical counterpart candidates. Combining thesedata with a photometric redshift catalog, we ruled out each candidate as thecounterpart to S190814bv and we placed deep, uniform limits on the opticalemission associated with S190814bv. For the nearest consistent GW distance,radiative transfer simulations of NSBH mergers constrain the ejecta mass ofS190814bv to be $M_\mathrm{ej} < 0.04$~$M_{\odot}$ at polar viewing angles, or$M_\mathrm{ej} < 0.03$~$M_{\odot}$ if the opacity is $\kappa <2$~cm$^2$g$^{-1}$. Assuming a tidal deformability for the neutron star at thehigh end of the range compatible with GW170817 results, our limits wouldconstrain the BH spin component aligned with the orbital momentum to be $ \chi< 0.7$ for mass ratios $Q < 6$, with weaker constraints for more compactneutron stars. We publicly release the photometry from this campaign athttp://www.astro.caltech.edu/~danny/static/s190814bv.

GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-Infrared Counterpart to a Neutron Star-Black Hole Merger