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Novel deep learning approach to detecting binary black hole mergers

Damon Beveridge1,*, Alistair McLeod1,†, Linqing Wen1,‡, and Andreas Wicenec2

  • *Contact author: damon.beveridge@research.uwa.edu.au
  • †Contact author: alistair.mcleod@research.uwa.edu.au
  • ‡Contact author: linqing.wen@uwa.edu.au
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Phys. Rev. D 111, 024005 – Published 3 January, 2025

DOI: https://doi.org/10.1103/PhysRevD.111.024005

Abstract

Gravitational wave detection has opened up new avenues for exploring and understanding some of the fundamental principles of the Universe. The optimal method for detecting modeled gravitational-wave events involves template-based matched filtering and performing a multidetector coincidence search in the resulting signal-to-noise ratio time series. In recent years, advancements in machine learning and deep learning have led to a flurry of research into using these techniques to replace matched filtering searches and for efficient and robust parameter estimation of the gravitational wave sources. This paper presents a feasibility study for a novel approach to detecting binary black hole gravitational wave signals, which utilizes deep learning techniques on the signal-to-noise ratio time series produced from matched filtering. We show that a deep-learning search can efficiently detect binary black hole gravitational waves from the signal-to-noise ratio time series in simulated Gaussian noise with simulated transient glitches. Furthermore, our search method can outperform a maximum SNR-based matched filtering search on simulated data of the Hanford and Livingston LIGO detectors in the presence of glitches. Lastly, since we are building upon the foundations of a matched filtering search pipeline, we can extract estimates for the signal-to-noise ratio and detector frame chirp mass of a gravitational wave event with similar accuracy as existing pipelines.

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Phys. Rev. D 111, 024005– Published 3 January, 2025
  • Received 17 August 2023
  • Revised 4 December 2024
  • Accepted 9 December 2024
Article part of CHORUS
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