2013/04/02 by The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration +1320 · 1 voice · 8 citations
Physics and Astronomy · #astro-ph.HE #gr-qc
paper · pdf · doi:10.1007/s41114-020-00026-9
published as Living Rev Relativ 23, 3 (2020) · 52 pages, 9 figures, 5 tables. We have updated the detector sensitivities (including the A+ and AdV+ upgrade); added expectations for binary black-holes, neutron-star black-holes, and intermediate-mass black holes; and added 3D volume localization expectations. This update is to change some numbers in Table 5 based on refinements to the simulations. Three authors were added
arxiv published 2013/04/02 · arxiv created 2020/11/24 · arxiv updated 2020/11/26
We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is BNS, NSBH, and BBH systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.