Upper Limits on the Rates of Binary Neutron Star and Neutron Star–black Hole Mergers from Advanced Ligo’s First Observing Run

We report here the non-detection of gravitational waves from the merger of binary–neutron star systems and neutron star–black hole systems during the first observing run of the Advanced Laser Interferometer Gravitationalwave Observatory (LIGO). In particular, we searched for gravitational-wave signals from binary–neutron star systems with component masses Î  M 1, 3 [ ] and component dimensionless spins <0.05. We also searched for neutron star–black hole systems with the same neutron star parameters, black hole mass Î  M 2, 99 [ ] , and no restriction on the black hole spin magnitude. We assess the sensitivity of the two LIGO detectors to these systems and find that they could have detected the merger of binary–neutron star systems with component mass distributions of 1.35±0.13Me at a volume-weighted average distance of ∼70Mpc, and for neutron star–black hole systems with neutron star masses of 1.4Me and black hole masses of at least 5Me, a volume-weighted average distance of at least ∼110Mpc. From this we constrain with 90% confidence the merger rate to be less than 12,600Gpcyr for binary–neutron star systems and less than 3600Gpcyr for neutron star–black hole systems. We discuss the astrophysical implications of these results, which we find to be in conflict with only the most optimistic predictions. However, we find that if no detection of neutron star–binary mergers is made in the next two Advanced LIGO and Advanced Virgo observing runs we would place significant constraints on the merger rates. Finally, assuming a rate of + 10 7 20 Gpc yr, short gamma-ray bursts beamed toward the Earth, and assuming that all short gamma-ray bursts have binary–neutron star (neutron star–black hole) progenitors, we can use our 90% confidence rate upper limits to constrain the beaming angle of the gamma-ray burst to be greater than  + 2 .3 1.1 1.7 (  + 4 .3 1.9 ).