scholarly journals Lensing magnification: gravitational waves from coalescing stellar-mass binary black holes

2021 ◽  
Vol 508 (1) ◽  
pp. 1253-1261
Author(s):  
Xikai Shan ◽  
Chengliang Wei ◽  
Bin Hu

ABSTRACT Gravitational waves (GWs) may be magnified or de-magnified due to lensing. This phenomenon will bias the distance estimation based on the matched filtering technique. Via the multi-sphere ray-tracing technique, we study the GW magnification effect and selection effect with particular attention to the stellar-mass binary black holes. We find that, for the observed luminosity distance $\lesssim 3\, \mathrm{Gpc}$, which is the aLIGO/Virgo observational horizon limit, the average magnification keeps as unity, namely unbiased estimation, with the relative distance uncertainty $\sigma (\hat{d})/\hat{d}\simeq 0.5{{\ \rm per\ cent}}\sim 1{{\ \rm per\ cent}}$. Beyond this observational horizon, the estimation bias can not be ignored, and with the scatters $\sigma (\hat{d})/\hat{d} = 1{{\ \rm per\ cent}}\sim 15{{\ \rm per\ cent}}$. Furthermore, we forecast these numbers for Einstein Telescope (ET). We find that the average magnification keeps closely as unity for the observed luminosity distance $\lesssim 90\, \mathrm{Gpc}$. The luminosity distance estimation error due to lensing for ET is about $\sigma (\hat{d})/\hat{d} \simeq 10{{\ \rm per\ cent}}$ for the luminosity distance $\gtrsim 25\, \mathrm{Gpc}$. Unlike the aLIGO/Virgo case, this sizable error is not due to the selection effect. It purely comes from the unavoidably accumulated lensing magnification. Moreover, we investigated the effects of the orientation angle and the BH mass distribution models. We found that the results are strongly dependent on these two components.

2020 ◽  
Vol 498 (3) ◽  
pp. 4287-4294
Author(s):  
Jongsuk Hong ◽  
Abbas Askar ◽  
Mirek Giersz ◽  
Arkadiusz Hypki ◽  
Suk-Jin Yoon

ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction based on clusters’ initial properties when the IMBH mass is not massive enough or the IMBH seed forms at a later time. However, binary black hole formation and subsequent merger events are significantly reduced compared to the prediction when the present-day IMBH mass is more massive than ${\sim}10^4\, \rm M_{\odot }$ or the present-day IMBH mass exceeds about 1 per cent of cluster’s initial total mass. By examining the maximum black hole mass in the system at the moment of black hole binary escaping, we find that ∼90 per cent of the merging binary black holes escape before the formation and growth of the IMBH. Furthermore, large fraction of stellar mass black holes are merged into the IMBH or escape as single black holes from globular clusters in cases of massive IMBHs, which can lead to the significant underpopulation of binary black holes merging with gravitational waves by a factor of 2 depending on the clusters’ initial distributions.


Author(s):  
Manuel Arca Sedda ◽  
Christopher P. L. Berry ◽  
Karan Jani ◽  
Pau Amaro-Seoane ◽  
Pierre Auclair ◽  
...  

AbstractSince 2015 the gravitational-wave observations of LIGO and Virgo have transformed our understanding of compact-object binaries. In the years to come, ground-based gravitational-wave observatories such as LIGO, Virgo, and their successors will increase in sensitivity, discovering thousands of stellar-mass binaries. In the 2030s, the space-based LISA will provide gravitational-wave observations of massive black holes binaries. Between the $\sim 10$ ∼ 10 –103 Hz band of ground-based observatories and the $\sim 10^{-4}$ ∼ 1 0 − 4 –10− 1 Hz band of LISA lies the uncharted decihertz gravitational-wave band. We propose a Decihertz Observatory to study this frequency range, and to complement observations made by other detectors. Decihertz observatories are well suited to observation of intermediate-mass ($\sim 10^{2}$ ∼ 1 0 2 –104M⊙) black holes; they will be able to detect stellar-mass binaries days to years before they merge, providing early warning of nearby binary neutron star mergers and measurements of the eccentricity of binary black holes, and they will enable new tests of general relativity and the Standard Model of particle physics. Here we summarise how a Decihertz Observatory could provide unique insights into how black holes form and evolve across cosmic time, improve prospects for both multimessenger astronomy and multiband gravitational-wave astronomy, and enable new probes of gravity, particle physics and cosmology.


2018 ◽  
Vol 98 (8) ◽  
Author(s):  
Roberto Cotesta ◽  
Alessandra Buonanno ◽  
Alejandro Bohé ◽  
Andrea Taracchini ◽  
Ian Hinder ◽  
...  

2020 ◽  
Vol 80 (11) ◽  
Author(s):  
Sai Wang ◽  
Zhi-Chao Zhao

AbstractA discovery of gravitational waves from binary black holes raises a possibility that measurements of them can provide strict tests of CPT invariance in gravitational waves. When CPT violation exists, if any, gravitational waves with different circular polarizations could gain a slight difference in propagating speeds. Hence, the birefringence of gravitational waves is induced and there should be a rotation of plus and cross modes. For CPT-violating dispersion relation $${\omega ^{2}=k^{2}}$$ ω 2 = k 2 $${\pm 2\zeta k^{3}}$$ ± 2 ζ k 3 , where a sign $${\pm }$$ ± denotes different circular polarizations, we find no substantial deviations from CPT invariance in gravitational waves by analyzing a compilation of ten signals of binary black holes in the LIGO-Virgo catalog GWTC-1. We obtain a strict constraint on the CPT-violating parameter, i.e., $$\zeta =0.14^{+0.22}_{-0.31}\times 10^{-15}\,\text {m}$$ ζ = 0 . 14 - 0.31 + 0.22 × 10 - 15 m , which is around two orders of magnitude better than the existing one. Therefore, this study stands for the up-to-date strictest tests of CPT invariance in gravitational waves.


2016 ◽  
Vol 93 (12) ◽  
Author(s):  
Collin Capano ◽  
Ian Harry ◽  
Stephen Privitera ◽  
Alessandra Buonanno

2007 ◽  
Vol 78 ◽  
pp. 012010 ◽  
Author(s):  
Joan M Centrella ◽  
John G Baker ◽  
William D Boggs ◽  
Bernard J Kelly ◽  
Sean T McWilliams ◽  
...  

2012 ◽  
Vol 85 (10) ◽  
Author(s):  
J. Abadie ◽  
B. P. Abbott ◽  
R. Abbott ◽  
T. D. Abbott ◽  
M. Abernathy ◽  
...  

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