2020
DOI: 10.1007/s41114-020-00026-9
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Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

Abstract: 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 V… Show more

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Cited by 689 publications
(432 citation statements)
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“…Future enhancements of the terrestrial gravitational wave detector network will improve our sensitivity to fainter gravitational wave signals, providing a valuable tool to prospect the expected population of galactic NSs in binary systems [48][49][50][51][52].…”
Section: Discussionmentioning
confidence: 99%
“…Future enhancements of the terrestrial gravitational wave detector network will improve our sensitivity to fainter gravitational wave signals, providing a valuable tool to prospect the expected population of galactic NSs in binary systems [48][49][50][51][52].…”
Section: Discussionmentioning
confidence: 99%
“…The characteristic speed of the ejecta is v eje /c 0.2−0.3 with a rest-mass of 10 −3 M ⊙ (see e.g., East et al, 2015;Foucart et al, 2015;Hayashi et al, 2020;Ruiz et al, 2020a). Therefore, the bolometric luminosity of kilonova signals is L knova 10 41 erg/s with rise times of 7 h. These luminosities correspond to an R band magnitude of ∼ 24 mag at 200 Mpc inside the aLIGO volume (Abbott et al, 2013), and above the LSST survey sensitivity of 24.5 mag (Barnes and Kasen, 2013;East et al, 2015). Hence some of these signals may be detectable by the LSST survey (Ruiz et al, 2020a).…”
Section: Nonmagnetized Evolutionsmentioning
confidence: 98%
“…When the observing run O4 starts with the GW detector network of the LIGO/Virgo/Kagra (LVK) collaboration, the predicted rate of BNS merger detections is 10 +52 −10 per year, their predicted median luminosity distance is 170 +6.3 −4.8 Mpc, and their predicted median 90% sky localisation area is 33 +4.9 −5.3 deg 2 (all values given as 5%-95% confidence intervals; Abbott et al 2020a). A 100-s iband exposure with SkyMapper can discover an GW170817-like kilonova at four times the distance of GW170817.…”
Section: Summary and Outlook To O4mentioning
confidence: 99%
“…The SkyMapper optical wide-field telescope in Australia (see Section 2.1) is one of the facilities that can discover early GW170817-like kilonovae and is probably the pivotal optical facility for events that occur in the Southern Sky between the end of the Chilean night and late in the Australian night. The size of the GW localisation area (a few hundred deg 2 , see Abbott et al 2020a) is usually much larger than the field of view (FoV) of our camera (5.7 deg 2 ). While the GW triggers in the third LIGO/Virgo observing run (O3) had a median localisation area of 4 480 deg 2 (Kasliwal et al 2020), the area shrinks quickly for events with stronger signals.…”
Section: Introductionmentioning
confidence: 99%