dc.contributor.author Abbott, B. P dc.contributor.author Abbott, R. dc.contributor.author Abbott, T. D dc.contributor.author Abraham, S. dc.contributor.author Acernese, F. dc.contributor.author Ackley, K. dc.contributor.author Adams, C. dc.contributor.author Adya, V. B dc.contributor.author Affeldt, C. dc.contributor.author Agathos, M. dc.contributor.author Agatsuma, K. dc.contributor.author Aggarwal, N. dc.contributor.author Aguiar, O. D dc.contributor.author Aiello, L. dc.contributor.author Ain, A. dc.contributor.author Ajith, P. dc.date.accessioned 2021-09-20T17:41:13Z dc.date.available 2021-09-20T17:41:13Z dc.date.issued 2020-09-28 dc.identifier.uri https://hdl.handle.net/1721.1/131976 dc.description.abstract Abstract en_US 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 binary neutron star, neutron star–black hole, and binary black hole 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. During O3, the median localization volume (90% credible region) is expected to be on the order of $$10^{5}, 10^{6}, 10^{7}\mathrm {\ Mpc}^3$$ 10 5 , 10 6 , 10 7 Mpc 3 for binary neutron star, neutron star–black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of $$1^{+12}_{-1}$$ 1 - 1 + 12 ( $$10^{+52}_{-10}$$ 10 - 10 + 52 ) for binary neutron star mergers, of $$0^{+19}_{-0}$$ 0 - 0 + 19 ( $$1^{+91}_{-1}$$ 1 - 1 + 91 ) for neutron star–black hole mergers, and $$17^{+22}_{-11}$$ 17 - 11 + 22 ( $$79^{+89}_{-44}$$ 79 - 44 + 89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers. dc.publisher Springer International Publishing en_US dc.relation.isversionof https://doi.org/10.1007/s41114-020-00026-9 en_US dc.rights Creative Commons Attribution en_US dc.rights.uri https://creativecommons.org/licenses/by/4.0/ en_US dc.source Springer International Publishing en_US dc.title Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA en_US dc.type Article en_US dc.identifier.citation Living Reviews in Relativity. 2020 Sep 28;23(1):3 en_US dc.identifier.mitlicense PUBLISHER_CC dc.eprint.version Final published version en_US dc.type.uri http://purl.org/eprint/type/JournalArticle en_US eprint.status http://purl.org/eprint/status/PeerReviewed en_US dc.date.updated 2021-01-10T04:15:06Z dc.language.rfc3066 en dc.rights.holder The Author(s) dspace.embargo.terms N dspace.date.submission 2021-01-10T04:15:06Z mit.license PUBLISHER_CC mit.metadata.status Authority Work and Publication Information Needed
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