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Gravitational waves from coalescences of neutron stars or stellar-mass blackholes into intermediate-mass black holes (IMBHs) of $\gtrsim 100$ solar massesrepresent one of the exciting possible sources for advanced gravitational-wavedetectors. These sources can provide definitive evidence for the existence ofIMBHs, probe globular-cluster dynamics, and potentially serve as tests ofgeneral relativity. We analyse the accuracy with which we can measure themasses and spins of the IMBH and its companion in intermediate-mass ratiocoalescences. We find that we can identify an IMBH with a mass above $100 ~M_\odot$ with $95\%$ confidence provided the massive body exceeds $130 ~M_\odot$. For source masses above $\sim200 ~ M_\odot$, the best measuredparameter is the frequency of the quasi-normal ringdown. Consequently, thetotal mass is measured better than the chirp mass for massive binaries, but thetotal mass is still partly degenerate with spin, which cannot be accuratelymeasured. Low-frequency detector sensitivity is particularly important formassive sources, since sensitivity to the inspiral phase is critical formeasuring the mass of the stellar-mass companion. We show that we canaccurately infer source parameters for cosmologically redshifted signals byapplying appropriate corrections. We investigate the impact of uncertainty inthe model gravitational waveforms and conclude that our main results are likelyrobust to systematics.

Inference on gravitational waves from coalescences of stellar-mass compact objects and intermediate-mass black holes