paper

Localization of Compact Binary Sources with Second Generation Gravitational-wave Interferometer Networks

arXiv:1909.12961 · doi:10.3847/1538-4357/abb373

Abstract

GW170817 began gravitational-wave multimessenger astronomy. However, GW170817 will not be representative of detections in the coming years -- typical gravitational-wave sources will be closer the detection horizon, have larger localization regions, and (when present) will have correspondingly weaker electromagnetic emission. In its design state, the gravitational-wave detector network in the mid-2020s will consist of up to five similar-sensitivity second-generation interferometers. The instantaneous sky-coverage by the full network is nearly isotropic, in contrast to the configuration during the first \change{three} observing runs. Along with the coverage of the sky, there are also commensurate increases in the average horizon for a given binary mass. We present a realistic set of localizations for binary neutron stars and neutron star--black hole binaries, incorporating intra-network duty cycles and selection effects on the astrophysical distributions. Based on the assumption of an duty cycle, and that two instruments observe a signal above the detection threshold, we anticipate a median of sq.\ deg.\ for binary neutron stars, and -- sq.\ deg.\ for neutron star--black hole (depending on the population assumed). These distributions have a wide spread, and the best localizations, even for networks with fewer instruments, will have localizations of -- sq.\ deg.\ range. The full five instrument network reduces localization regions to a few tens of degrees at worst.

20 pages, 8 figures, 3 tables, accepted in ApJ

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