Black Hole Mass Scaling Relations for Early-type Galaxies. I. M_BH–M_{*, sph} and M_BH–M_*,gal

Abstract

Analyzing a sample of 84 early-type galaxies (ETGs) with directly measured supermassive black hole massesnearly doubling the sample size of such galaxies with multicomponent decompositions-a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals M M BH ,sph 1.27 0.07 * µ  with a total scatter of Δ rms =0.52dex in the M log BH ( ) direction. Importantly, however, we discover that the ES/S0-type galaxies with disks are offset from the E-type galaxies by more than a factor of ten in their M M BH ,sph * ratio, with ramifications for formation theories, simulations, and some virial factor measurements used to convert AGN virial masses into M BH . Separately, each population follows a steeper relation with slopes of 1.86±0.20 and 1.90±0.20, respectively. The offset mass ratio is mainly due to the exclusion of the disk mass, with the two populations offset by only a factor of two in their M M BH ,gal * ratio in the M BH -M ,gal * diagram where M M BH ,gal 1.8 0.2 * µ  and 0.6 0.1 rms D =  dex depending on the sample. For M M 10 BH 7  , we detect no significant bend nor offset in either the M BH -M ,sph * or M BH -M ,gal * relations due to barred versus non-barred, or core-Sérsic versus Sérsic, ETGs. For reference, the ensemble of late-type galaxies (which invariably are Sérsic galaxies) follow M BH -M ,sph * and M BH -M ,gal * relations with slopes equal to 2.16±0.32 and 3.05±0.70, respectively. Finally, we provide some useful conversion coefficients, υ, accounting for the different stellar mass-to-light ratios used in the literature, and we report the discovery of a local, compact massive spheroid in NGC5252.

No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5

“…Our sample of AGNs tend to lie below the Kormendy & Ho (2013) relation for local inactive early-type galaxies at a given M stellar . It appears that the local M BH − M stellar relation of Davis et al (2018) is consistent with our data, even though only based on late-type galaxies, while the relation of Sahu et al (2019), which is only based on early-type galaxies, seems to be inconsistent with our high-redshift AGNs. Shankar et al (2016) proposed the local intrinsic relation by correcting the selection bias in the M BH − M stellar relation of inactive BHs with dynamically-measured masses.…”

Black hole feedback and the evolution of massive early-type galaxies

“…Second, changes in velocity dispersion are also associated with changes in the internal structure of galaxies (e.g. Graham & Scott 2013;Sahu et al 2019) and even due to changes in orientation (e.g. Xiao et al 2011).…”

Quantifying the Effect of Black Hole Feedback from the Central Galaxy on the Satellite Populations of Groups and Clusters

“…First, at fixed stellar velocity dispersion, there are apparent differences in black hole mass (Martín-Navarro et al 2016), i.e., the intrinsic scatter in the M • -σ relation is not zero (Beifiori et al 2012). Second, the relation between black hole mass and stellar velocity dispersion might change with galaxy mass, internal structure, and even orientation (Xiao et al 2011;Graham & Scott 2013;Martín-Navarro & Mezcua 2018;Sahu et al 2019), which implies that trends with halo mass might be biased (Bernardi et al 2007). These uncertainties and systematics related to the use of the velocity dispersion as a proxy for black hole mass support our use of a running-median to separate over-massive and undermassive black hole halos, which in practice has no other meaning than differentiating the two populations, acknowledging our lack of information about the actual black hole masses.…”