Dynamical Assembly of GW sources: Theoretical Models and New Observations

The recent discoveries by LIGO/Virgo have uncovered a binary black hole (BBH) merger distribution described by a variety of masses, spins, and possible orbital eccentricity, which hints for a rich underlying distribution of astrophysical formation mechanisms. The question is, how do we observationally tell these apart? Are the majority of BBH mergers formed dynamically, or through isolated binary evolution? I will in this talk present recent work on the unique observables resulting from different dynamical channels, and compare these to a couple of recent GW observations. A few ideas targeting next generation GW-observatories will also be presented.