The Supermassive Black Hole Mass–spheroid Stellar Mass Relation for Sérsic and Core-Sérsic Galaxies

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-Sersic and Sersic galaxies, we find that they are described by very different M BH-M sph, * relations. For core-Sersic galaxies - which are typically massive and luminous, with M BH 2 x 108 M-sun - we find M BH , consistent with other literature relations. However, for the Sersic galaxies - with typically lower masses, M sph, * 3 x 1010 M-sun - we find , a dramatically steeper slope that differs by more than 2 standard deviations. This relation confirms that, for Sersic galaxies, M BH is not a constant fraction of M sph, *. Sersic 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-Sersic galaxies, where the black hole and spheroid grow in lockstep. We have additionally compared our Sersic 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.