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We explore for the first time the effect of self-interacting dark matter(SIDM) on the dark matter (DM) and baryonic distribution in massive galaxiesformed in hydrodynamical cosmological simulations, including explicit baryonicphysics treatment. A novel implementation of Super-Massive Black Hole (SMBH)formation and evolution is used, as in Tremmel et al.(2015, 2016), allowing toexplicitly follow SMBH dynamics at the center of galaxies. A high SIDM constantcross-section is chosen, $\sigma$=10 $\rm cm^2/gr$, to amplify differences fromCDM models. Milky Way-like galaxies form a shallower DM density profile in SIDMthan they do in CDM, with differences already at 20 kpc scales. Thisdemonstrates that even for the most massive spirals the effect of SIDMdominates over the adiabatic contraction due to baryons. Strikingly, thedynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massivespirals have sunk to the centre of their host galaxy in both the SIDM and CDMrun, while in less massive galaxies about 80$\%$ of the SMBH population isoff-centered in the SIDM case, as opposed to the CDM case in which $\sim$90$\%$of SMBHs have reached their host's centre. SMBHs are found as far as $\sim$9kpc away from the centre of their host SIDM galaxy. This difference is due tothe increased dynamical friction timescale caused by the lower DM density inSIDM galaxies compared to CDM, resulting in 'core stalling'. This pilot workhighlights the importance of simulating in a full hydrodynamical contextdifferent DM models combined to SMBH physics to study their influence on galaxyformation.

A rumble in the dark: signatures of self-interacting dark matter in Super-Massive Black Hole dynamics and galaxy density profiles