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We present a high resolution numerical study of the sinking and merging ofmassive black holes (MBHs) with masses in the range of $10^3 - 10^7 \,\mathrm{M}_\odot$ in multiple minor mergers of low mass dark matter haloswithout and with galaxies ($4\times 10^8 \, \mathrm{M}_\odot \lesssim\mathrm{M}_{\mathrm{halo}} \lesssim 2\times 10^{10} \, \mathrm{M}_\odot)$. TheKetju simulation code, a combination of the Gadget tree solver with accurateregularised integration, uses unsoftened forces between the star/dark mattercomponents and the MBHs for an accurate treatment of dynamical friction andscattering of dark matter/stars by MBH binaries or multiples. Post-Newtoniancorrections up to order 3.5 for MBH interactions allow for coalescence bygravitational wave emission and gravitational recoil kicks. Low mass MBHs($\lesssim 10^5 \, \mathrm{M}_\odot$) hardly sink to the centre or merge.Sinking MBHs have various complex evolution paths - binaries, triplets,free-floating MBHs, and dynamically or recoil ejected MBHs. Collisionalinteractions with dark matter alone can drive MBHs to coalescence. The highestmass MBHs of $\gtrsim 10^6 M_\odot$ mostly sink to the centre and trigger thescouring of dark matter and stellar cores. The scouring can transform acentrally baryon dominated system to a dark matter dominated system. Ouridealized high-resolution study highlights the difficulty to bring in and keeplow mass MBHs in the centres of low mass halos/galaxies - a remaining challengefor merger assisted MBH seed growth mechanisms.

The difficult path to coalescence: massive black hole dynamics in merging low mass dark matter haloes and galaxies