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The two interferometric LIGO gravitational-wave observatories provide themost sensitive data to date to study the gravitational-wave Universe. As partof a global network, they have just completed their third observing run inwhich they observed many tens of signals from merging compact binary systems.It has long been known that a limiting factor in identifying transientgravitational-wave signals is the presence of transient non-Gaussian noise,which reduce the ability of astrophysical searches to detect signalsconfidently. Significant efforts are taken to identify and mitigate this noiseat the source, but its presence persists, leading to the need for softwaresolutions. Taking a set of transient noise artefacts categorised by theGravitySpy software during the O3a observing era, we produce parameterisedpopulation models of the noise projected into the space of astrophysical modelparameters of merging binary systems. We compare the inferred populationproperties of transient noise artefacts with observed astrophysical systemsfrom the GWTC2.1 catalogue. We find that while the population of astrophysicalsystems tend to have near equal masses and moderate spins, transient noiseartefacts are typically characterised by extreme mass ratios and large spins.This work provides a new method to calculate the consistency of an observedcandidate with a given class of noise artefacts. This approach could be used inassessing the consistency of candidates found by astrophysical searches (i.e.determining if they are consistent with a known glitch class). Furthermore, theapproach could be incorporated into astrophysical searches directly,potentially improving the reach of the detectors, though only a detailed studywould verify this.

Parameterised population models of transient non-Gaussian noise in the LIGO gravitational-wave detectors