Abstract:
The final phase of the coalescence of compact binaries consisting of Neutron stars and/or Black Holes produce Gravitational Waves (GWs) that are strong enough to fall inside the detectability range of our current ground-based GW detectors. For a sufficiently large observed GW transient sample, their frequency and nature of occurrence should directly relate to the properties and distribution of the underlying compact remnants that gave rise to them and therefore to the population of their stellar progenitors......
