Speaker
Description
In this talk, we consider the problem of measuring the flat-LCDM parameters using binary black hole coalescences observed by third-generation (3G) gravitational-wave detectors like the Einstein Telescope and Cosmic Explorer. Using simulated dark sirens together with redshift information from a realistic simulated galaxy catalog, we adopt a Bayesian framework to jointly estimate the Hubble constant $H_0$ and the matter energy density parameter $\Omega_m$ in different scenarios. Assuming a galaxy catalog complete up to $z=1$ and using dark sirens detected with a network signal-to-noise ratio greater than 300, we show that a network made of ET and two CEs can constrain $H_0$ ($\Omega_m$) to a promising 0.7% (9.0%) at 90% CI in one year of full observation. We also explore the importance of single-host dark sirens and an optimistic scenario with a galaxy catalog complete up to $z=3$.
