# A Search for Optical Emission from Binary-Black-Hole Merger GW170814 with the Dark Energy Camera

## TL;DR

This study conducted a comprehensive optical search for electromagnetic counterparts to the binary black hole merger GW170814 using the Dark Energy Camera, finding no associated optical emission and setting constraints on such emissions.

## Contribution

First to perform an extensive optical search for EM counterparts to GW170814 with the Dark Energy Camera covering 86% of the probable sky area.

## Key findings

- No optical counterparts detected within the search parameters.
- Disfavors bright, rapidly fading optical emission from BBH mergers.
- Provides the most complete optical counterpart search for BBH mergers to date.

## Abstract

Binary black hole (BBH) mergers found by the LIGO and Virgo detectors are of immense scientific interest to the astrophysics community, but are considered unlikely to be sources of electromagnetic emission. To test whether they have rapidly fading optical counterparts, we used the Dark Energy Camera to perform an $i$-band search for the BBH merger GW170814, the first gravitational wave detected by three interferometers. The 87-deg$^2$ localization region (at 90\% confidence) centered in the Dark Energy Survey (DES) footprint enabled us to image 86\% of the probable sky area to a depth of $i\sim 23$ mag and provide the most comprehensive dataset to search for EM emission from BBH mergers. To identify candidates, we perform difference imaging with our search images and with templates from pre-existing DES images. The analysis strategy and selection requirements were designed to remove supernovae and to identify transients that decline in the first two epochs. We find two candidates, each of which is spatially coincident with a star or a high-redshift galaxy in the DES catalogs, and they are thus unlikely to be associated with GW170814. Our search finds no candidates associated with GW170814, disfavoring rapidly declining optical emission from BBH mergers brighter than $i\sim 23$ mag ($L_{\rm optical} \sim 5\times10^{41}$ erg/s) 1-2 days after coalescence. In terms of GW sky map coverage, this is the most complete search for optical counterparts to BBH mergers to date