tokens: use the results of a double-Sérsic fitting to the surface density profile of our simulated galaxy, as described in Section 4.2 (the values are given in Table 2 ). Eris BH sits well below both relations, even though the black hole seeds start off close to the extrapolation at lower masses of the MBH-stellar mass relation (coloured bullets in the left-hand panel): this is because the black hole accretion rates are much lower than what would be required to keep up with the star formation rate in the central region (see Fig. 3 ). Figure 7. M BH – M Star and M BH – M Bulge relations. The red and blue symbols are from a compilation of Erwin Gadotti ( 2012 ) for early-type and late-type galaxies, respectively (with fits for the M BH – M Bulge relation shown by the dashed lines). The orange diamond is the location of the Milky Way in the plane as reported by Erwin Gadotti ( 2012 ). The yellow circle indicates the location of Eris BH . The coloured bulletts in the M BH − M Star figure show the location of the seeds, colour-coded as in Fig. 1 Table 2. Summary of global properties of Eris BH and Eris at z = 0. The stellar and gas masses in columns 1 and 2 refer to the total stellar and gas masses within the halo, also used to calculate the baryon fractions given in column 3. The disc and bulge masses have been obtained fitting a double Sérsic profile to the face-on surface density profile, with scale lengths given in columns 8 and 9. The last column gives the Sérsic index for the bulge, while the Sérsic index for the disc has been fixed to unity. Masses are given in solar masses, distances in kpc and velocities in km s − 1 . Having only one simulation, we can not give quantitative predictions on whether black holes in pseudobulges follow a different relation with the properties of the host (or if they do not follow any relation at all). But we note that our results on the M BH –σ and M BH – M Bulge relations are both consistent with what is found by Greene et al. ( 2008 ), and could also fit within the picture drawn by Kormendy et al. ( 2011 ), given the slow Seyfert-like growth of our simulated black hole. 4 BLACK HOLE FEEDBACK AND ITS EFFECTS ON THE HOST GALAXY As described in Section 2.2.2 , the simulation includes also a prescription for black hole feedback: a fraction of the energy extracted in the accretion process couples thermally with the surrounding medium. This standard prescription has been used extensively in other works, and its effects led to the idea of a ‘self-regulation’ of black hole growth to explain the origin of the M BH –σ relation and the ejection of gas from the host galaxy and the resulting quenching of star formation (e.g. Di Matteo et al. 2005 ). Given that the accretion rates are generally quite small for the central black hole of our simulated galaxy, we expect the effects of feedback to be modest. We find, in fact, that the amount of energy released by the black hole is significantly lower than the one released by
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