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The two binary black-hole (BBH) coalescences detected by LIGO, GW150914 andGW151226, were relatively nearby sources, with a redshift of ~0.1. As thesensitivity of Advanced LIGO and Virgo increases in the next few years, theywill eventually detect stellar-mass BBHs up to redshifts of ~1. However, theseare still relatively small distances compared with the size of the Universe, orwith those encountered in most areas of astrophysics. In order to study BBHduring the epoch of reionization, or black holes born from population IIIstars, more sensitive instruments are needed. Third-generationgravitational-wave detectors, such as the Einstein Telescope or the CosmicExplorer are already in an advanced R&D stage. These detectors will be roughlya factor of 10 more sensitive in strain than the current generation, and beable to detect BBH mergers beyond a redshift of 20. In this paper we quantifythe precision with which these new facilities will be able to estimate theparameters of stellar-mass, heavy, and intermediate-mass BBH as a function oftheir redshifts and the number of detectors. We show that having only twodetectors would result in relatively poor estimates of black hole intrinsicmasses; a situation improved with three or four instruments. Largerimprovements are visible for the sky localization, although it is not yet clearwhether BBHs are luminous in the electromagnetic or neutrino band. Themeasurement of the spin parameters, on the other hand, do not improvesignificantly as more detectors are added to the network since redshiftinformation are not required to measure spin.

Parameter estimation for binary black holes with networks of third generation gravitational-wave detectors