2013ApJ...768...76S

We have examined the relationship between supermassive black hole mass (M_BH) and the stellar mass of the host spheroid (M_sph, *_) for a sample of 75 nearby galaxies. To derive the spheroid stellar masses we used improved Two Micron All Sky Survey K_s-band photometry from the ARCHANGEL photometry pipeline. Dividing our sample into core-Sérsic and Sérsic galaxies, we find that they are described by very different M_BH-M_sph, *_relations. For core-Sérsic galaxies–which are typically massive and luminous, with M_BH ≳ 2x10⁸ M_☉–we find M_BH∝ M^0.97±0.14_sph,*, consistent with other literature relations. However, for the Sérsic galaxies–with typically lower masses, M_sph, *_ ≲ 3x10¹⁰ M_☉–we find M_BH∝ M^2.22±0.58_sph,*, a dramatically steeper slope that differs by more than 2 standard deviations. This relation confirms that, for Sérsic galaxies, M_BH is not a constant fraction of M_sph, *_. Sérsic galaxies can grow via the accretion of gas which fuels both star formation and the central black hole, as well as through merging. Their black hole grows significantly more rapidly than their host spheroid, prior to growth by dry merging events that produce core-Sérsic galaxies, where the black hole and spheroid grow in lockstep. We have additionally compared our Sérsic M_BH-M_sph, *_ relation with the corresponding relation for nuclear star clusters, confirming that the two classes of central massive object follow significantly different scaling relations.