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Binary black holes occupy a special place in our quest for understanding theevolution of galaxies along cosmic history. If massive black holes grow at thecenter of (pre-)galactic structures that experience a sequence of mergerepisodes, then dual black holes form as inescapable outcome of galaxy assembly.But, if the black holes reach coalescence, then they become the loudest sourcesof gravitational waves ever in the universe. Nature seems to provide a pathwayfor the formation of these exotic binaries, and a number of key questions needto be addressed: How do massive black holes pair in a merger? Depending on theproperties of the underlying galaxies, do black holes always form a closeKeplerian binary? If a binary forms, does hardening proceed down to the domaincontrolled by gravitational wave back reaction? What is the role played by gasand/or stars in braking the black holes, and on which timescale doescoalescence occur? Can the black holes accrete on flight and shine during theirpathway to coalescence? N-Body/hydrodynamical codes have proven to be vitaltools for studying their evolution, and progress in this field is expected togrow rapidly in the effort to describe, in full realism, the physics of starsand gas around the black holes, starting from the cosmological large scale of amerger. If detected in the new window provided by the upcoming gravitationalwave experiments, binary black holes will provide a deep view into the processof hierarchical clustering which is at the heart of the current paradigm ofgalaxy formation. They will also be exquisite probes for testing GeneralRelativity, as the theory of gravity. The waveforms emitted during theinspiral, coalescence and ring-down phase carry in their shape the sign of adynamically evolving space-time and the proof of the existence of an horizon.

Massive Binary Black Holes in the Cosmic Landscape