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Multi-frequency gravitational wave (GW) observations are useful probes of theformation processes of coalescing stellar-mass binary black holes (BBHs). Wediscuss the phase drift in the GW inspiral waveform of the merging BBH causedby its center-of-mass acceleration. The acceleration strongly depends on thelocation where a BBH forms within a galaxy, allowing observations of the earlyinspiral phase of LIGO-like BBH mergers by the Laser Interferometer SpaceAntenna (LISA) to test the formation mechanism. In particular, BBHs formed indense nuclear star clusters or via compact accretion disks around a nuclearsupermassive black hole in active galactic nuclei would suffer strongacceleration, and produce large phase drifts measurable by LISA. The hostgalaxies of the coalescing BBHs in these scenarios can also be uniquelyidentified in the LISA error volume, without electromagnetic counterparts. Anon-detection of phase drifts would rule out or constrain the contribution ofthe nuclear formation channels to the stellar-mass BBH population.

physical review. d/physical review. d.

Probing stellar binary black hole formation in galactic nuclei via the  imprint of their center of mass acceleration on their gravitational wave  signal