Speaker
Description
With sensitivity improvements of next-generation (XG) gravitational-wave detectors, we expect to resolve >99% of binary black hole (BBH) mergers across the Universe and roughly half of all binary neutron star (BNS) mergers. Detecting a cosmological stochastic background in the presence of such astrophysical foregrounds is therefore challenging and calls for robust statistical methodology.
I will present a two-step framework: (i) identify and remove resolvable BBH signals in the time–frequency domain, and (ii) perform a joint analysis that simultaneously fits the remaining BNS foreground and the cosmological GW background (CGWB). In addition, I will quantify the impact of shot noise arising from finite observation time and occasional nearby loud events on the analysis, present a mitigation strategy, and estimate the resulting sensitivity reduction.