Limits on the Electromagnetic Counterpart to S190814bv. (arXiv:2001.05436v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Watson_A/0/1/0/all/0/1">Alan M. Watson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Butler_N/0/1/0/all/0/1">Nathaniel R. Butler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_W/0/1/0/all/0/1">William H. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becerra_R/0/1/0/all/0/1">Rosa L. Becerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereyra_M/0/1/0/all/0/1">Margarita Pereyra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angeles_F/0/1/0/all/0/1">Fernando Angeles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farah_A/0/1/0/all/0/1">Alejandro Farah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Figueroa_L/0/1/0/all/0/1">Liliana Figueroa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Buitrago_D/0/1/0/all/0/1">Diego Gonz&#xe1;lez-Buitrago</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quiros_F/0/1/0/all/0/1">Fernando Quir&#xf3;s</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruiz_Diaz_Soto_J/0/1/0/all/0/1">Jaime Ru&#xed;z-D&#xed;az-Soto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vergas_C/0/1/0/all/0/1">Carlos Tejada de Vergas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tinoco_S/0/1/0/all/0/1">Silvio J. Tinoco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolfram_T/0/1/0/all/0/1">Tanner Wolfram</a>

We derive limits on any electromagnetic counterpart to the compact binary
merger S190814bv, whose parameters are consistent with the merger of a black
hole and a neutron star. We present observations with the new wide-field
optical imager DDOTI and also consider Swift/BAT observations reported by
Palmer et al. (2019). We show that Swift/BAT would have detected a counterpart
with similar properties to a typical on-axis short GRB at the 98 per cent
confidence level, whereas our DDOTI observations only rule out such a
counterpart at the 27 per cent confidence level. Neither have sufficient
sensitivity to rule out an off-axis counterpart like GW 170817. We compare the
efficiency of Swift/BAT and DDOTI for future observations, and show that DDOTI
is likely to be about twice as efficient as Swift/BAT for off-axis events up to
about 100 Mpc.

We derive limits on any electromagnetic counterpart to the compact binary
merger S190814bv, whose parameters are consistent with the merger of a black
hole and a neutron star. We present observations with the new wide-field
optical imager DDOTI and also consider Swift/BAT observations reported by
Palmer et al. (2019). We show that Swift/BAT would have detected a counterpart
with similar properties to a typical on-axis short GRB at the 98 per cent
confidence level, whereas our DDOTI observations only rule out such a
counterpart at the 27 per cent confidence level. Neither have sufficient
sensitivity to rule out an off-axis counterpart like GW 170817. We compare the
efficiency of Swift/BAT and DDOTI for future observations, and show that DDOTI
is likely to be about twice as efficient as Swift/BAT for off-axis events up to
about 100 Mpc.

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