Pith. sign in

REVIEW 3 cited by

Subtracting Compact Binary Foregrounds to Search for Subdominant Gravitational-Wave Backgrounds in Next-Generation Ground-Based Observatories

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 2209.01310 v2 pith:DBQ7O7LO submitted 2022-09-03 gr-qc astro-ph.HEhep-ph

Bei Zhou , Luca Reali , Emanuele Berti , Mesut Çal{i}şkan , Cyril Creque-Sarbinowski , Marc Kamionkowski , B. S. Sathyaprakash This is my paper · ORCID
classification gr-qcastro-ph.HEhep-ph
keywords sgwbsotherbackgroundbinarygravitational-wavenext-generationobservatoriesresidual
verification ladder T0 review T1 audit T2 compute T3 formal
0 comments
read the original abstract

Stochastic gravitational-wave backgrounds (SGWBs) derive from the superposition of numerous individually unresolved gravitational-wave (GW) signals. Detecting SGWBs provides us with invaluable information about astrophysics, cosmology, and fundamental physics. In this paper, we study SGWBs from binary black-hole (BBH) and binary neutron-star (BNS) coalescences in a network of next-generation ground-based GW observatories (Cosmic Explorer and Einstein Telescope) and determine how well they can be measured; this then limits how well we can observe other subdominant astrophysical and cosmological SGWBs. We simulate all-Universe populations of BBHs and BNSs and calculate the corresponding SGWBs, which consist of a superposition of (i) undetected signals, and (ii) the residual background from imperfect removal of resolved sources. The sum of the two components sets the sensitivity for observing other SGWBs. Our results show that, even with next-generation observatories, the residual background is large and limits the sensitivity to other SGWBs. The main contributions to the residual background arise from uncertainties in inferring the coalescence phase and luminosity distance of the detected signals. Alternative approaches to signal subtraction would need to be explored to minimize the BBH and BNS foreground in order to observe SGWBs from other subdominant astrophysical and cosmological sources.

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. All You Need is not $\Omega_\mathrm{gw}$: Beyond the Mean of the Cross-Correlation Estimator when Searching for an Astrophysical Gravitational-Wave Background

    gr-qc 2026-08 conditional novelty 6.0 of 10

    For a two-detector Cosmic Explorer network, the cross-correlation estimator of the binary black hole background has skewness 0.31 and excess kurtosis 1.3 at 20 Hz, a non-Gaussianity that will matter for next-generatio...

  2. A "Neutrino Fog" For Gravitational Waves: The Stochastic Gravitational Wave Background from Supernova Neutrino Memory

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    Using 3D supernova simulations, the authors predict that neutrino memory creates a gravitational wave background with Omega_GW around 1e-16 at 0.1 Hz, within reach of future space-based detectors.

  3. Can machine learning improve the detectability and disentanglement of the gravitational-wave background?

    gr-qc 2026-07 conditional novelty 5.0 of 10

    On 108 days of simulated O4a-like LIGO noise, a deep-learning autoencoder plus MCMC pipeline detects a CBC background at Ωα≈4.5e-9 and separates a flat cosmological component at Ω0≈9e-10, outperforming the standard py...

Pith tools