Sensing and vetoing loud transient noises for the gravitational-wave detection

TL;DR

This paper reviews gravitational-wave detection methods, sources, and noise suppression techniques, emphasizing the importance of sensing and vetoing loud transient noises to enhance detection sensitivity and data quality.

Contribution

It provides a comprehensive overview of detection algorithms, noise sources, and noise mitigation strategies, highlighting recent advancements in gravitational-wave observatory data analysis.

Findings

Summary of gravitational-wave sources and detection principles

Overview of noise sources and their impact on detection sensitivity

Description of algorithms for noise suppression and data quality monitoring

Abstract

Since the first detection of gravitational-wave (GW), GW150914, September 14th 2015, the multi-messenger astronomy added a new way of observing the Universe together with electromagnetic (EM) waves and neutrinos. After two years, GW together with its EM counterpart from binary neutron stars, GW170817 and GRB170817A, has been observed. The detection of GWs opened a new window of astronomy/astrophysics and will be an important messenger to understand the Universe. In this article, we briefly review the gravitational-wave and the astrophysical sources and introduce the basic principle of the laser interferometer as a gravitational-wave detector and its noise sources to understand how the gravitational-waves are detected in the laser interferometer. Finally, we summarize the search algorithms currently used in the gravitational-wave observatories and the detector characterization algorithms used to suppress noises and to monitor data quality in order to improve the reach of the astrophysical searches.