Estimating $H_0$ in non-stationary noise

Gravitational-wave observations of binary neutron star mergers and their optical counterparts provide an independent measurement of $H_0$. Therefore, a thorough understanding of the source of systematic uncertainty for gravitational-wave observations is crucial. Estimating the properties of gravitational-wave signals measured by ground-based detectors requires an understanding of the characteristics of the detector noise. The most commonly used likelihood assumes that the noise is Gaussian and stationary. However, data from ground-based detectors can be highly non-stationary, which means the broadband detector noise can change on the order of tens of seconds. Variations in the detector noise could bias the estimation of the properties of the gravitational-wave sources. This talk will characterize how non-stationary noise affects the parameter estimation of gravitational-wave signals in LIGO and Virgo data from the third observing run and how this may affect the estimation of $H_0$.