RELATIONS BETWEEN CENTRAL BLACK HOLE MASS AND TOTAL GALAXY STELLAR MASS IN THE LOCAL UNIVERSE

By A. Reines, M. Volonteri. 2015

308 citations recorded by the source corpus.

Scaling relations between central black hole (BH) mass and host galaxy properties are of fundamental importance to studies of BH and galaxy evolution throughout cosmic time. Here we investigate the relationship between BH mass and host galaxy total stellar mass using a sample of 262 broad-line active galactic nuclei (AGNs) in the nearby universe (z < 0.055), as well as 79 galaxies with dynamical BH masses. The vast majority of our AGN sample is constructed using Sloan Digital Sky Survey spectroscopy and searching for Seyfert-like narrow-line ratios and broad Hα emission. BH masses are estimated using standard virial techniques. We also include a small number of dwarf galaxies with total stellar masses Mstellar ≲ 109.5 M⊙ and a subsample of the reverberation-mapped AGNs. Total stellar masses of all 341 galaxies are calculated in the most consistent manner feasible using color-dependent mass-to-light ratios. We find a clear correlation between BH mass and total stellar mass for the AGN host galaxies, with MBH ∝ Mstellar, similar to that of early-type galaxies with dynamically detected BHs. However, the relation defined by the AGNs has a normalization that is lower by more than an order of magnitude, with a BH-to-total stellar mass fraction of MBH/Mstellar ∼ 0.025% across the stellar mass range 108 ≤ Mstellar/M⊙ ≤ 1012. This result has significant implications for studies at high redshift and cosmological simulations in which stellar bulges cannot be resolved.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/24670557e4e6be9a5a0f9954f1c6bddc2bc6a85a

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Citations in the corpus

Gravitational torque-driven black hole growth and feedback in cosmological simulations (2016, background): “M relations of Reines & Volonteri (2015) for AGN and inactive galaxies separately, where MBH is related to the total stellar mass of galaxies as opposed to the bulge mass. Black holes with initial mass Mseed = 105 M h−1 were placed at the centre of galaxies as they first reached M ≈ 103 Mseed in…”
Blossoms from black hole seeds: properties and early growth regulated by supernova feedback (2016, methodology): “1), the simulated BHs connect to the local galaxy sample of Reines & Volonteri (2015) (Fig.”
Nuclear star clusters (2009, unknown): “…Spengler et al. (2017), (41) Walcher et al. (2005), (42) Bland-Hawthorn and Gerhard (2016), (43) Williams et al. (2017), (44) Seth et al. (2010), (45) Reines and Volonteri (2015), (46) Cappellari et al. (2013), (47) McConnachie (2012), (48) derived from Jarrett et al. (2003), (49) Karachentsev…”
The cosmic evolution of massive black holes in the Horizon-AGN simulation (2016, methodology): “Recently, Reines & Volonteri (2015) re-analysed in as much consistent a way as possible the sample of local BHs with dynamical mass measurements (Kormendy & Ho 2013), and also include BHs in AGN with mass measured through reverberation mapping (Bentz & Katz 2015), as well as a sample of broad-line…”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale (2017, methodology): “Using the stellar mass of NGC 4993, inferred from our SED modeling (Section 5), and the relation of Reines & Volonteri (2015), we infer a supermassive black hole mass of ~M 10BH 8.5 M .”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “The typical mass ratio is ~M M 0.002BH host (e.g., Marconi & Hunt 2003; Häring & Rix 2004; Sani et al. 2011; Kormendy & Ho 2013; a factor ∼10 lower according to Reines & Volonteri 2015).”
The dark nemesis of galaxy formation : why hot haloes trigger black hole growth and bring star formation to an end (2016, background): “By estimating black hole masses from the emission line widths, Reines & Volonteri (2015) give us a glimpse of the relation at lower masses.”
Supermassive black holes and their feedback effects in the IllustrisTNG simulation (2017, background): “…e.g. the SMBH mass with the bulge mass (or velocity dispersion) of the host (Magorrian et al. 1998; Tremaine et al. 2002; Häring & Rix 2004; McConnell & Ma 2013; Kormendy & Ho 2013; Graham & Scott 2015; Reines & Volonteri 2015; Savorgnan et al. 2016), indicates a connection between the two objects.”
Constraining Stellar-mass Black Hole Mergers in AGN Disks Detectable with LIGO (2017, background): “The NGN upper limit corresponds to dwarf galaxies with stellar mass >109Me (Baldry et al. 2012), which includes all locally observed SMBH ( 105Me) inferred from M−σ studies of galaxies and dwarf galaxies (Reines & Volonteri 2015).”
Observational evidence for intermediate-mass black holes (2017, background): “…hosting SMBHs is directly connected to the formation of seed BHs: the low-mass end of the MBH − σ∗ correlation (or also of the MBH − M∗ relation; Reines & Volonteri 2015) is expected to flatten towards what looks like a plume of ungrown BHs if seed BHs are massive (i.e. formed from…”
The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs (2016, background): “There is also evidence that the relationships break down at low redshift for lower mass, star forming galaxies (Reines & Volonteri 2015).”
Primordial black holes as generators of cosmic structures (2018, background): “There is also the well-known correlation between by the mass of the SMBH and mass of the bulge, with the ratio being of order 104 (Graham 2012; Sun et al. 2013; Reines & Volonteri 2015), although there may also be a correlation with the mass of the dark halo (Bogdan & Goulding 2015).”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, methodology): “Recently Reines & Volonteri (2015) have compiled a sample of 262 broad-line AGN atz 0.055 which roughly overlaps in volume with the dynamical mass black hole samples we have been discussing so far.”