  We investigate detection prospects of the gravitational-wave background (GWB)
that originates from the merging of compact objects formed by the collapse of
population III stars. Younger population I/II stars lead to a GWB in the
LIGO/Virgo frequency band at the inspiral phase, while population III stars
would likely show up at the later merger and ringdown phases. We show that,
using a network of third-generation detectors, we may be able to separate a
population I/II signal from a population III one, provided we can subtract
individual coalescence events. A detection of a population III GWB could reveal
important information, such as the average redshifted total mass.
