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Massive black hole (MBH) coalescences are powerful sources of low-frequencygravitational waves. To study these events in the cosmological context we needto trace the large-scale structure and cosmic evolution of a statisticalpopulation of galaxies, from dim dwarfs to bright galaxies. To cover such alarge range of galaxy masses, we analyse two complementary simulations:Horizon-AGN with a large volume and low resolution which tracks the high-mass(> 1e7 Msun) MBH population, and NewHorizon with a smaller volume but higherresolution that traces the low-mass (< 1e7 Msun) MBH population. WhileHorizon-AGN can be used to estimate the rate of inspirals for Pulsar TimingArrays, NewHorizon can investigate MBH mergers in a statistical sample of dwarfgalaxies for LISA, which is sensitive to low-mass MBHs. We use the same methodto analyse the two simulations, post-processing MBH dynamics to account fortime delays mostly determined by dynamical friction and stellar hardening. Inboth simulations, MBHs typically merge long after the galaxies do, so that thegalaxy morphology at the time of the MBH merger is no longer determined by thegalaxy merger from which the MBH merger originated. These time delays cause aloss of high-z MBH coalescences, shifting the peak of the MBH merger rate toz~1-2. This study shows how tracking MBH mergers in low-mass galaxies iscrucial to probing the MBH merger rate for LISA and investigate the propertiesof the host galaxies.

Black hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations