Host galaxy identification for binary black hole mergers with long baseline gravitational wave detectors

Howell, E. J.; Chan, M.; Chu, Q.; Jones, D. Heath; Heng, I. S.; Lee, Hyung Mok; Blair, David; Degallaix, J.; Regimbau, T.; Miao, H.; Zhao, C.; Hendry, M.; Coward, D. M.; Messenger, C.; Li, Ju; Zhu, Zong-Hong

doi:10.1093/mnras/stx3077

Cited by 10 publications

(9 citation statements)

References 72 publications

(56 reference statements)

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“…The benefits of building a large network of GW detectors including Australia and China have been widely discussed [32,88,89]. The advantages of multi-detector networks for the localization of GW sources have been studied in a previous work [32] for BBHs with component masses larger than 12 M .…”

Section: Network Of Three and Four Detectorsmentioning

confidence: 99%

Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology

Zhao¹,

2018

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We use the Fisher information matrix to investigate the angular resolution and luminosity distance uncertainty for coalescing binary neutron stars (BNSs) and neutron star-black hole binaries (NSBHs) detected by the third-generation (3G) gravitational-wave (GW) detectors. Our study focuses on an individual 3G detector and a network of up to four 3G detectors at different locations including the US, Europe, China and Australia for the proposed Einstein Telescope (ET) and Cosmic Explorer (CE) detectors. We in particular examine the effect of the Earth's rotation, as GW signals from BNS and low mass NSBH systems could be hours long for 3G detectors. In this case, an individual detector can be effectively treated as a detector network with long baselines formed by the trajectory of the detector as it rotates with the Earth. Therefore, a single detector or two-detector networks could also be used to localize the GW sources effectively. We find that, a time-dependent antenna beam-pattern function can help better localize BNS and NSBH sources, especially those edge-on ones. The medium angular resolution for one ET-D detector is around 150 deg 2 for BNSs at a redshift of z = 0.1, which improves rapidly with a decreasing low-frequency cutoff f low in sensitivity. The medium angular resolution for a network of two CE detectors in the US and Europe respectively is around 20 deg 2 at z = 0.2 for the simulated BNS and NSBH samples. While for a network of two ET-D detectors, the similar angular resolution can be achieved at a much higher redshift of z = 0.5. The angular resolution of a network of three detectors is mainly determined by the baselines between detectors regardless of the CE or ET detector type. The medium angular resolution of BNS for a network of three detectors of the ET-D or CE type in the US, Europe and Australia is around 10 deg 2 at z = 2. We discuss the implications of our results to multi-messenger astronomy and in particular to using GW sources as independent tools to constrain the Hubble constant H0, the deceleration parameter q0 and the equation-of-state (EoS) of dark energy. We find that in general, if 10 BNSs or NSBHs at z = 0.1 with known redshifts are detected by 3G networks consisting of two ET-like detectors, H0 can be measured with an accuracy of 0.9%. If 1000 face-on BNSs at z < 2 are detected with known redshifts, we are able to achieve ∆q0 = 0.002 for deceleration parameter, or ∆w0 = 0.03 and ∆wa = 0.2 for EoS of dark energy, respectively.

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Section: Network Of Three and Four Detectorsmentioning

confidence: 99%

Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology

Zhao¹,

2018

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“…For O3 and aLIGO design we assume noise curve with SensMon ranges of 120 Mpc and 173 Mpc respectively; the sources of our noise curves are described in Appendix A. Table 2 outlines the horizon distances (as a benchmark) and following (Howell et al 2018) relative distances 50% and 90% of BNS mergers will be detected. It is interesting to note that although a future configuration such as Voyager has an optimal reach of 2.4 Gpc, the efficiency at that range will be negligible.…”

Section: Bns Detection Efficiencymentioning

confidence: 99%

Joint gravitational wave – gamma-ray burst detection rates in the aftermath of GW170817

Howell

Ackley

Rowlinson

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The observational follow-up campaign of the gravitational wave (GW) multi-messenger event GW170817/GRB170817A has shown that the prompt γ-rays are consistent with a relativistic structured jet observed from a wide viewing angle 20 • . We perform Bayesian inference using the data from early and late EM observations to determine the jet profile of GRB170817A assuming a structured jet model. We use the geometric dependence on the burst luminosity to produce a short duration gamma-ray burst (sGRB) efficiency function with redshift, which folded in with binary neutron star detection rate, allows us to estimate the future joint GW/sGRB detection rates for LIGO and Virgo detectors. We show that, if the jet structured profile of GRB170817A is a relatively common feature of sGRBs, then there is a realistic probability of another off-axis coincident detection during the third aLIGO/Virgo observing run (O3). We also find that up to 4 yr −1 joint events may be observed during the advanced LIGO run at design sensitivity and up to 10 yr −1 by the upgraded advanced LIGO configuration A+. We show that the detection efficiencies for wide-angled sGRB emissions will be limited by GRB satellites as the GW detection range increases through proposed upgrades. Therefore, although the number of coincident detections will increase with GW detector sensitivity, the relative proportion of detected binary neutron stars with γ-ray counterparts will decrease; 11% for O3 down to 2% during A+.

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“…For a sGRB detection efficiency function we assumed Fermi-GBM and used well cited parameters for the sGRB LF [5], folding in the geometric dependence based on our model parameters of a structured jet. For the GW detection efficiency functions we used the framework of [13] for a range of aLIGO sensitivities and proposed upgrades. Table 1 shows the derived BNS detection rates.…”

Section: Joint Gw/sgrb Detection Ratesmentioning

confidence: 99%

Joint gravitational wave - gamma-ray burst detection rates in the aftermath of GW170817

Howell¹,

Ackley²,

Rowlinson³

et al. 2019

Proceedings of the New Era of Multi-Messenger Astrophysics — PoS(Asterics2019)

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The observational follow-up campaign of the gravitational wave (GW) multi-messenger event GW170817/GRB170817A has shown that the prompt γ-rays are consistent with a relativistic structured jet observed from a wide viewing angle. We model the structured jet profile of GRB170817A assuming a structured jet model to estimate the future joint GW/sGRB detection rates for LIGO and Virgo detectors. We show that, if the jet structured profile of GRB170817A is a relatively common feature of sGRBs, then there is a realistic probability of another off-axis coincident detection during the third aLIGO/Virgo observing run (O3). We also find that up to 4 yr −1 joint events may be observed during the advanced LIGO run at design sensitivity and up to 10 yr −1 by the upgraded advanced LIGO configuration A+. We show that the detection efficiencies for wide-angled sGRB emissions will be limited by GRB satellites as the GW detection range increases through proposed upgrades. Therefore, although the number of coincident detections will increase with GW detector sensitivity, the relative proportion of detected binary neutron stars with γ-ray counterparts will decrease; 11% for O3 down to 2% during A+.

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Host galaxy identification for binary black hole mergers with long baseline gravitational wave detectors

Cited by 10 publications

References 72 publications

Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology

Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology

Joint gravitational wave – gamma-ray burst detection rates in the aftermath of GW170817

Joint gravitational wave - gamma-ray burst detection rates in the aftermath of GW170817

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