Time-dependence of the astrophysical stochastic gravitational wave background

Mukherjee, Suvodip; Silk, Joseph

doi:10.1093/mnras/stz3226

Cited by 60 publications

(42 citation statements)

References 56 publications

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“…We should be able to unveil the population of high redshift GW sources. it should also be possible to explore the time dependence of the stochastic GW background (Mukherjee & Silk 2019. This could provide an independent means of distinguishing between different kinds of sources contributing in the stochastic GW background.…”

Section: Forecast For the Ligo/virgo And A+ Sensitivitymentioning

confidence: 99%

“…Measurement of the stochastic GW background (even in the absence of a detection) can probe the high redshift merger rate and its evolution with redshift (Mukherjee & Silk 2019;Boco et al 2019;Callister et al 2020). Using data from the third observational run, LIGO/Virgo has estimated the stochastic GW background power spectrum (Abbott et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Can we distinguish astrophysical from primordial black holes via the stochastic gravitational wave background?

Mukherjee,

Silk

2021

Preprint

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One of the crucial windows for distinguishing astrophysical black holes from primordial black holes is through the redshift evolution of their respective merger rates. The low redshift population of black holes of astrophysical origin is expected to follow the star formation rate. The corresponding peak in their merger rate is going to peak at a redshift smaller than that of the star formation rate peak (z p ≈ 2), depending on the time delay between the formation and mergers of black holes. Black holes of primordial origin are going to be present before the formation of the stars, and the merger rate of these sources at high redshift is going to be large. We propose joint estimation of a hybrid merger rate from the stochastic gravitational wave background, which can use the cosmic history of merger rates to distinguish between the two populations of black holes. Using the latest bounds on the amplitude of the stochastic gravitational wave background amplitude from the third observation run of LIGO/Virgo, we obtain weak constraints at 68% C.L. on the primordial black hole merger rate index 2.56 +1.64 −1.76 and astrophysical black hole time delay 6.7 +4.22 −4.74 Gyr. We should be able to distinguish between the different populations of black holes with the forthcoming O5 and A+ detector sensitivities.

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Section: Forecast For the Ligo/virgo And A+ Sensitivitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Can we distinguish astrophysical from primordial black holes via the stochastic gravitational wave background?

Mukherjee,

Silk

2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…It is worth pointing out that these observational features of astrophysical backgrounds discussed here may themselves provide insight in compact binary population parameters such as binary coalescence rates for different binary species, as detailed in [128]. Furthermore, the time dependence of astrophysical backgrounds in general may be a powerful discriminating factor between these and backgrounds of primordial origin.…”

Section: Observational Properties Of Stochastic Backgroundsmentioning

confidence: 81%

“…Correlating anisotropies in the GWB which electromagnetic observations has also been proposed as a target for future detectors. In some cases, this means using galaxy catalogues to guide the model used for anisotropic GWB searches [242], while in other cases, the proposal is to correlate sub-threshold GW signals with EM transients to probe fundamental physics [128,331].…”

Section: Stochastic Searches With Third Generation Interferometersmentioning

confidence: 99%

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Renzini¹,

Goncharov²,

Jenkins³

et al. 2022

Preprint

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The collection of individually resolvable gravitational wave (GW) events makes up a tiny fraction of all GW signals that reach our detectors, while most lie below the confusion limit and are undetected. Similarly to voices in a crowded room, the collection of unresolved signals gives rise to a background that is well-described via stochastic variables and, hence, referred to as the stochastic GW background (SGWB). In this review, we provide an overview of stochastic GW signals and characterise them based on features of interest such as generation processes and observational properties. We then review the current detection strategies for stochastic backgrounds, offering a ready-to-use manual for stochastic GW searches in real data. In the process, we distinguish between interferometric measurements of GWs, either by ground-based or space-based laser interferometers, and timing-residuals analyses with pulsar timing arrays (PTAs). These detection methods have been applied to real data both by large GW collaborations and smaller research groups, and the most recent and instructive results are reported here. We close this review with an outlook on future observations with third generation detectors, space-based interferometers, and potential noninterferometric detection methods proposed in the literature.

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“…Besides the frequency dependence, there are other properties that distinguish the nature of different backgrounds, such as their anisotropies (Cusin et al 2018;Jenkins et al 2018Jenkins et al , 2019Cusin et al 2019b;Bertacca et al 2020;Pitrou et al 2020), polarizations (Cusin et al 2019a), and popcorn (sometimes referred as non-Gaussian or time-dependent) signal (Coward & Regimbau 2006;Regimbau & Mandic 2008;Wu et al 2012;Mukherjee & Silk 2020). Those characteristics would be essential for disentangling different possible sources and identifying the origin of the SGWB.…”

Section: Introductionmentioning

confidence: 99%

Tracking the origin of black holes with the stochastic gravitational wave background popcorn signal

Braglia¹,

García-Bellido²,

Kuroyanagi³

2022

Preprint

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Unresolved sources of gravitational waves (GWs) produced by the merger of a binary of black holes at cosmological distances combine into a stochastic background. Such a background is in the continuous or popcorn regime, depending on whether the GW rate is high enough so that two or more events overlap in the same frequency band. These two regimes respectively correspond to large and small values of the so-called duty cycle. We study the detection regime of the background in models of Primordial Black Holes (PBHs) and compare it to the one produced by black holes of stellar origin. Focusing on ground-based detectors, we show that the duty cycle of the PBH-origin background is larger than that of astrophysical black holes because of differences in their mass function and the merger rate. Our study opens up the possibility to learn about the primordial or astrophysical nature of black hole populations by examining the statistical properties of the stochastic background.

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Time-dependence of the astrophysical stochastic gravitational wave background

Cited by 60 publications

References 56 publications

Can we distinguish astrophysical from primordial black holes via the stochastic gravitational wave background?

Can we distinguish astrophysical from primordial black holes via the stochastic gravitational wave background?

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Tracking the origin of black holes with the stochastic gravitational wave background popcorn signal

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