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A search for the isotropic stochastic background using data from Advanced LIGO's second observing run

The LIGO Scientific Collaboration, The Virgo Collaboration, Matas, A., & Dvorkin, I. (in preparation). A search for the isotropic stochastic background using data from Advanced LIGO's second observing run.

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1903.02886.pdf (Preprint), 5MB
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Creators:
The LIGO Scientific Collaboration, Author
The Virgo Collaboration, Author
Matas, Andrew1, Author
Dvorkin, Irina1, Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
Abstract: The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study we present the results from a cross-correlation analysis on data from Advanced LIGO's second observing run (O2), which we combine with the results of the first observing run (O1). We do not find evidence for a stochastic background, so we place upper limits on the normalized energy density in gravitational waves at the 95% credible level of $\Omega_{\rm GW}<6.0\times 10^{-8}$ for a frequency-independent (flat) background and $\Omega_{\rm GW}<4.8\times 10^{-8}$ at 25 Hz for a background of compact binary coalescences. The upper limit improves over the O1 result by a factor of 2.8. Additionally, we place upper limits on the energy density in an isotropic background of scalar- and vector-polarized gravitational waves, and we discuss the implication of these results for models of compact binaries and cosmic string backgrounds. Finally, we present a conservative estimate of the correlated broadband noise due to the magnetic Schumann resonances in O2, based on magnetometer measurements at both the LIGO Hanford and LIGO Livingston observatories. We find that correlated noise is well below the O2 sensitivity.

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Dates: 2019-03-07
Publication Status: Not specified
Pages: 14 pages, 8 figures
Publishing info: -
Rev. Method: -
Identifiers: arXiv: 1903.02886
URI: http://arxiv.org/abs/1903.02886
Degree: -

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