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Upper limits on the isotropic gravitational-wave background from the first part of LIGO, Virgo, and KAGRA’s fourth observing run
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Upper limits on the isotropic gravitational-wave background from the first part of LIGO, Virgo, and KAGRA’s fourth observing run

A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, D. Adhikari, N. Adhikari, R. X. Adhikari, V. K. Adkins, …
Physical Review D, 卷.114(4), 042001
08/2026
DOI: https://doi.org/10.1103/wq57-sjt2

摘要

We present results from the search for an isotropic gravitational-wave background using Advanced LIGO and Advanced Virgo data from O1 through O4a, the first part of the fourth observing run. This background is the accumulated signal from unresolved sources throughout cosmic history and encodes information about the merger history of compact binaries throughout the Universe, as well as exotic physics and potentially primordial processes from the early cosmos. Our cross-correlation analysis reveals no statistically significant background signal, enabling us to constrain several theoretical scenarios. For compact binary coalescences which approximately follow a 2 / 3 power-law spectrum, we constrain the fractional energy density to Ω GW ( 25 Hz ) ≤ 2.0 × 10 − 9 (95% credibility), a factor of 1.7 improvement over previous results. Scale-invariant backgrounds are constrained to Ω GW ( 25 Hz ) ≤ 2.8 × 10 − 9 , representing a 2.1 × sensitivity gain. We also place new limits on alternative gravity theories predicting nonstandard polarization modes and confirm that terrestrial magnetic noise sources remain below our detection threshold. Combining these spectral limits with population models for Gravitational-Wave Transient Catalog (GWTC)-4, the latest gravitational-wave event catalog, we find our constraints remain above predicted merger backgrounds but are approaching detectability. The joint analysis combining the background limits shown here with GWTC-4 enables improved inference of the binary black hole merger rate evolution across cosmic time. Furthermore, employing GWTC-4 inference results and standard modeling choices, we estimate that the total background arising from compact binary coalescences is Ω CBC ( 25 Hz ) = 0.9 − 0.5 + 1.1 × 10 − 9 at 90% confidence, where the largest contribution is due to binary black holes only, Ω BBH ( 25 Hz ) = 0.8 − 0.5 + 1.1 × 10 − 9 .

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