Chirp mass based glitch identification in long-duration gravitational-wave detection

The data from the ground-based interferometric gravitational-wave (GW) detectors is often plagued by highly localized short-duration glitches which pose a serious challenge for any transient GW search. These glitches are not of any astrophysical origin but rather arise due to environmental or instrumental artifacts. In this work, we propose a glitch identification algorithm for the scenario of presence of a glitch, occurring within 20 s before or 10 s after the merger time of a coalescing compact binary system with chirp mass less than or equal to $5M_{\odot }$. We devise the chirp mass consistency parameter across different Q-planes in the Q-transform. We test this algorithm using a variety of short-duration glitches from the first and second observational runs of Advanced LIGO and Virgo detectors in the simulations with long-duration binary inspiral signal. The demonstration of this glitch identification algorithm in the simulated signals of generic low mass and low eccentricity binary systems shows the direct application of it in the long-duration unmodeled searches.

Figure 1

Q-transform of an injected signal of $1.4M_{\odot }–1.4M_{\odot }$ in presence of a blip.

Figure 2

Q-transforms of some different types of blips from O1-O2 data used for our study.

Figure 3

Energy variation of signals and glitches with respect to different Q-values.

Figure 4

Cumulative distribution for D for all the signal and glitch bins. The black (red) distribution represents the glitch (signal) bins.

Figure 5

$\mathrm{\Delta }t$ distribution for glitches from the simulation study.

Figure 6

(a) Variation of $\mathrm{\Delta }t$ with glitch SNR. (b) Identification of the glitch from the GW170817 data using our algorithm.