2016/07/25 by The LIGO Scientific Collaboration, the Virgo Collaboration, B. P. Abbott +960 · 4 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Binary black hole #Black hole (networking) #Computer science #Galaxy #Gamma-ray bursts and supernovae #Gravitational wave #LIGO #Neutron star #Physics #Pulsars and Gravitational Waves Research #Stellar black hole #Stellar evolution #Stellar mass loss #X-ray binary #X-ray burster #astro-ph.CO #astro-ph.HE #gr-qc
paper · pdf · doi:10.3847/2041-8205/832/2/l21
17 pages, 8 figures
arxiv created 2016/07/25 · openalex created_date 2016/08/23 · openalex publication_date 2016/11/23 · arxiv updated 2016/12/14 · openalex updated_date 2026/08/06
ABSTRACT 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 Gravitational-wave Observatory (LIGO). In particular, we searched for gravitational-wave signals from binary–neutron star systems with component masses and component dimensionless spins <0.05. We also searched for neutron star–black hole systems with the same neutron star parameters, black hole mass , 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 ± 0.13 M ⊙ at a volume-weighted average distance of ∼70 Mpc, and for neutron star–black hole systems with neutron star masses of 1.4 M ⊙ and black hole masses of at least 5 M ⊙ , a volume-weighted average distance of at least ∼110 Mpc. From this we constrain with 90% confidence the merger rate to be less than 12,600 Gpc −3 yr −1 for binary–neutron star systems and less than 3600 Gpc −3 yr −1 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 Gpc −3 yr −1 , 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 ( ).