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Improved limits on a stochastic gravitational-wave background and its anisotropies from Advanced LIGO O1 and O2 runs

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arxiv 1907.10329 v1 pith:NFHRYCPH submitted 2019-07-24 gr-qc astro-ph.COastro-ph.IM

Arianna Renzini , Carlo Contaldi This is my paper · ORCID
classification gr-qcastro-ph.COastro-ph.IM
keywords backgroundlimitsstochasticdataomegaadvancedanisotropiesestimate
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abstract

We integrate the entire, publicly available, Advanced LIGO (ALIGO) data set to obtain maximum-likelihood constraint maps of the Stochastic Gravitational-Wave Background (SGWB). From these we derive limits on the energy density of the stochastic background $\Omega_{\rm GW}$, and its anisotropy. We find 95% confident limits $\Omega_{\rm GW} < 5.2\times 10^{-8}$ at $50$ Hz for a spectral index $\alpha=2/3$ consistent with a stochastic background due to inspiral events and $\Omega_{\rm GW} < 3.2\times 10^{-7}$ for a scale (frequency) invariant spectrum. We also report upper limits on the angular power spectra $C_\ell$ for three broadband integrations of the data. Finally we present an estimate where we integrate the data into ten separate spectral bins as a first attempt to carry out a model-independent estimate the SGWB and its anisotropies.

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Cited by 2 Pith papers

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

  1. Directional Search for Persistent Gravitational Waves: Results from the First Part of LIGO-Virgo-KAGRA's Fourth Observing Run

    gr-qc 2025-10 conditional novelty 6.0 of 10

    An 8.3-year LIGO–Virgo–KAGRA search for persistent, direction-dependent gravitational waves finds no signal and yields the most restrictive upper limits to date on anisotropic backgrounds and targeted sources.

  2. Estimating the gravitational wave background anisotropy: a Bayesian approach boosted by cross-correlation angular power spectrum

    astro-ph.CO 2024-12 conditional novelty 6.0 of 10

    A new likelihood function estimates GWB anisotropy angular power spectra directly from detector data, and cross-correlation with the CMB can make the quadrupole measurable with four years of LISA data.

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