A search for optical and near-infrared counterparts of the compact binary merger GW190814. (arXiv:2007.04998v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Thakur_A/0/1/0/all/0/1">A. L. Thakur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dichiara_S/0/1/0/all/0/1">S. Dichiara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Troja_E/0/1/0/all/0/1">E. Troja</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chase_E/0/1/0/all/0/1">E. A. Chase</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Ramirez_R/0/1/0/all/0/1">R. Sanchez-Ramirez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_L/0/1/0/all/0/1">L. Piro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fryer_C/0/1/0/all/0/1">C. L. Fryer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Butler_N/0/1/0/all/0/1">N. R. Butler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Watson_A/0/1/0/all/0/1">A. M. Watson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wollaeger_R/0/1/0/all/0/1">R. T. Wollaeger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ambrosi_E/0/1/0/all/0/1">E. Ambrosi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_J/0/1/0/all/0/1">J. Becerra Gonz&#xe1;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becerra_R/0/1/0/all/0/1">R. L. Becerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruni_G/0/1/0/all/0/1">G. Bruni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cenko_B/0/1/0/all/0/1">B. S. Cenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cusumano_G/0/1/0/all/0/1">G. Cusumano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAi_A/0/1/0/all/0/1">Antonino D&#x27;A&#xec;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Durbak_J/0/1/0/all/0/1">J. Durbak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fontes_C/0/1/0/all/0/1">C. J. Fontes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gatkine_P/0/1/0/all/0/1">P. Gatkine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hungerford_A/0/1/0/all/0/1">A. L. Hungerford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korobkin_O/0/1/0/all/0/1">O. Korobkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kutyrev_A/0/1/0/all/0/1">A. S. Kutyrev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_W/0/1/0/all/0/1">W. H. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lotti_S/0/1/0/all/0/1">S. Lotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minervini_G/0/1/0/all/0/1">G. Minervini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novara_G/0/1/0/all/0/1">G. Novara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parola_V/0/1/0/all/0/1">V. La Parola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereyra_M/0/1/0/all/0/1">M. Pereyra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_R/0/1/0/all/0/1">R. Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tiengo_A/0/1/0/all/0/1">A. Tiengo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veilleux_S/0/1/0/all/0/1">S. Veilleux</a>

We report on our observing campaign of the compact binary merger GW190814,
detected by the Advanced LIGO and Advanced Virgo detectors on August 14th,
2019. This signal has the best localisation of any observed gravitational wave
(GW) source, with a 90% probability area of 18.5 deg$^2$, and an estimated
distance of ~ 240 Mpc. We obtained wide-field observations with the Deca-Degree
Optical Transient Imager (DDOTI) covering 88% of the probability area down to a
limiting magnitude of $w$ = 19.9 AB. Nearby galaxies within the high
probability region were targeted with the Lowell Discovery Telescope (LDT),
whereas promising candidate counterparts were characterized through
multi-colour photometry with the Reionization and Transients InfraRed (RATIR)
and spectroscopy with the Gran Telescopio de Canarias (GTC). We use our optical
and near-infrared limits in conjunction with the upper limits obtained by the
community to constrain the possible electromagnetic counterparts associated
with the merger. A gamma-ray burst seen along its jet’s axis is disfavoured by
the multi-wavelength dataset, whereas the presence of a burst seen at larger
viewing angles is not well constrained. Although our observations are not
sensitive to a kilonova similar to AT2017gfo, we can rule out high-mass (> 0.1
M$_{odot}$) fast-moving (mean velocity >= 0.3c) wind ejecta for a possible
kilonova associated with this merger.

We report on our observing campaign of the compact binary merger GW190814,
detected by the Advanced LIGO and Advanced Virgo detectors on August 14th,
2019. This signal has the best localisation of any observed gravitational wave
(GW) source, with a 90% probability area of 18.5 deg$^2$, and an estimated
distance of ~ 240 Mpc. We obtained wide-field observations with the Deca-Degree
Optical Transient Imager (DDOTI) covering 88% of the probability area down to a
limiting magnitude of $w$ = 19.9 AB. Nearby galaxies within the high
probability region were targeted with the Lowell Discovery Telescope (LDT),
whereas promising candidate counterparts were characterized through
multi-colour photometry with the Reionization and Transients InfraRed (RATIR)
and spectroscopy with the Gran Telescopio de Canarias (GTC). We use our optical
and near-infrared limits in conjunction with the upper limits obtained by the
community to constrain the possible electromagnetic counterparts associated
with the merger. A gamma-ray burst seen along its jet’s axis is disfavoured by
the multi-wavelength dataset, whereas the presence of a burst seen at larger
viewing angles is not well constrained. Although our observations are not
sensitive to a kilonova similar to AT2017gfo, we can rule out high-mass (> 0.1
M$_{odot}$) fast-moving (mean velocity >= 0.3c) wind ejecta for a possible
kilonova associated with this merger.

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