Substructure in black hole scaling diagrams and implications for the coevolution of black holes and galaxies

2019 ◽  
Vol 15 (S359) ◽  
pp. 37-39
Author(s):  
Benjamin L. Davis ◽  
Nandini Sahu ◽  
Alister W. Graham
Keyword(s):  
Black Hole ◽  
Stellar Mass ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Physical Processes ◽  
Stellar Velocity ◽  
Galaxy Sample ◽  
Evolutionary Paths ◽  
Black Hole Masses

AbstractOur multi-component photometric decomposition of the largest galaxy sample to date with dynamically-measured black hole masses nearly doubles the number of such galaxies. We have discovered substantially modified scaling relations between the black hole mass and the host galaxy properties, including the spheroid (bulge) stellar mass, the total galaxy stellar mass, and the central stellar velocity dispersion. These refinements partly arose because we were able to explore the scaling relations for various sub-populations of galaxies built by different physical processes, as traced by the presence of a disk, early-type versus late-type galaxies, or a Sérsic versus core-Sérsic spheroid light profile. The new relations appear fundamentally linked with the evolutionary paths followed by galaxies, and they have ramifications for simulations and formation theories involving both quenching and accretion.

scholarly journals Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

2019 ◽  
Vol 625 ◽  
pp. A62 ◽  
Author(s):  
Sabine Thater ◽  
Davor Krajnović ◽  
Michele Cappellari ◽  
Timothy A. Davis ◽  
P. Tim de Zeeuw ◽  
...  
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Velocity Dispersion ◽  
Variable Mass ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Early Type ◽  
Black Hole Mass ◽  
The Impact ◽  
Black Hole Masses

Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.

scholarly journals A Local Baseline of the Black Hole Mass Scaling Relations for Active Galaxies. IV. Correlations Between M BH and Host Galaxy σ, Stellar Mass, and Luminosity

2021 ◽  
Vol 921 (1) ◽  
pp. 36
Author(s):  
Vardha N. Bennert ◽  
Tommaso Treu ◽  
Xuheng Ding ◽  
Isak Stomberg ◽  
Simon Birrer ◽  
...  
Keyword(s):  
Black Hole ◽  
Stellar Mass ◽  
Active Galaxies ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Mass Scaling

Probing black hole - host galaxy scaling relations with obscured type II AGN

2019 ◽  
Vol 15 (S356) ◽  
pp. 365-365
Author(s):  
Dalya Baron
Keyword(s):  
Black Hole ◽  
Cosmic Time ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Type I ◽  
Type Ii ◽  
Black Hole Mass ◽  
Ionization State ◽  
Line Region ◽  
Black Hole Masses

AbstractThe scaling relations between supermassive black holes and their host galaxy properties are of fundamental importance in the context black hole-host galaxy co-evolution throughout cosmic time. Beyond the local universe, such relations are based on black hole mass estimates in type I AGN. Unfortunately, for this type of objects the host galaxy properties are more difficult to obtain since the AGN dominates the observed flux in most wavelength ranges. In this poster I will present a new correlation we discovered between the narrow L([OIII])/L(Hβ) line ratio and the FWHM(broad Hα). This scaling relation ties the kinematics of the gas clouds in the broad line region to the ionization state of gas in the narrow line region, connecting the properties of gas clouds kiloparsecs away from the black hole to material gravitationally bound to it on sub-parsec scales. This relation can be used to estimate black hole masses from narrow emission lines only, and thus brings the missing piece required to estimate black hole masses in obscured type II AGN. Using this technique, we estimate the black hole mass of about 10,000 type II AGN, and present, for the first time, M(BH)-sigma and M(BH)-M(stars) scaling relations for this population. These relations are remarkably consistent with those observed for type I AGN, suggesting that this new method may perform as reliably as the classical estimate used in non-obscured type I AGN. These findings open a new window for studies of black hole-host galaxy co-evolution throughout cosmic time.

A LOCAL BASELINE OF THE BLACK HOLE MASS SCALING RELATIONS FOR ACTIVE GALAXIES. II. MEASURING STELLAR VELOCITY DISPERSION IN ACTIVE GALAXIES

2012 ◽  
Vol 201 (2) ◽  
pp. 29 ◽  
Author(s):  
Chelsea E. Harris ◽  
Vardha N. Bennert ◽  
Matthew W. Auger ◽  
Tommaso Treu ◽  
Jong-Hak Woo ◽  
...  
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Active Galaxies ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Mass Scaling ◽  
Stellar Velocity

scholarly journals REVISITING THE SCALING RELATIONS OF BLACK HOLE MASSES AND HOST GALAXY PROPERTIES

2013 ◽  
Vol 764 (2) ◽  
pp. 184 ◽  
Author(s):  
Nicholas J. McConnell ◽  
Chung-Pei Ma
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Black Hole Masses

scholarly journals Exploring black hole scaling relations via the ensemble variability of Active Galactic Nuclei

2021 ◽  
Author(s):  
A Georgakakis ◽  
I Papadakis ◽  
M Paolillo
Keyword(s):  
Black Hole ◽  
Galactic Nuclei ◽  
Stellar Mass ◽  
Mass Relation ◽  
Black Hole Mass ◽  
X Ray ◽  
Mass Scaling ◽  
Spectrum Density ◽  
First Time ◽  
Black Hole Masses

Abstract An empirical model is presented that links, for the first time, the demographics of AGN to their ensemble X-ray variability properties. Observations on the incidence of AGN in galaxies are combined with (i) models of the Power Spectrum Density (PSD) of the flux variations of AGN and (ii) parameterisations of the black hole mass versus stellar-mass scaling relation, to predict the mean excess variance of active black hole populations in cosmological volumes. We show that the comparison of the model with observational measurements of the ensemble excess variance as a function of X-ray luminosity provides a handle on both the PSD models and the black hole mass versus stellar mass relation. We find strong evidence against a PSD model that is described by a broken power-law and a constant overall normalization. Instead our analysis indicates that the amplitude of the PSD depends on the physical properties of the accretion events, such as the Eddington ratio and/or the black hole mass. We also find that current observational measurements of the ensemble excess variance are consistent with the black hole mass versus stellar mass relation of local spheroids based on dynamically determined black hole masses. We also discuss future prospects of the proposed approach to jointly constrain the PSD of AGN and the black hole mass versus stellar mass relation as a function of redshift.

Quasar black hole masses and accretion rates across cosmic time

2019 ◽  
Vol 15 (S359) ◽  
pp. 57-61
Author(s):  
Michael Brotherton ◽  
Jaya Maithil ◽  
Adam Myers ◽  
Ohad Shemmer ◽  
Brandon Matthews ◽  
...  
Keyword(s):  
Black Hole ◽  
High Redshift ◽  
Cosmic Time ◽  
Small Samples ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Reverberation Mapping ◽  
Scaling Relationships ◽  
Accretion Rates ◽  
Black Hole Masses

AbstractQuasar black hole masses are most commonly estimated using broad emission lines in single epoch spectra based on scaling relationships determined from reverberation mapping of small samples of low-redshift objects. Several effects have been identified requiring modifications to these scaling relationships, resulting in significant reductions of the black hole mass determinations at high redshift. Correcting these systematic biases is critical to understanding the relationships among black hole and host galaxy properties. We are completing a program using the Gemini North telescope, called the Gemini North Infrared Spectrograph (GNIRS) Distant Quasar Survey (DQS), that has produced rest-frame optical spectra of about 200 high-redshift quasars (z = 1.5–3.5). The GNIRS-DQS will produce new and improved ultraviolet-based black hole mass and accretion rate prescriptions, as well as new redshift prescriptions for velocity zero points of high-z quasars, necessary to measure feedback.

On the host galaxy properties of stellar binary black hole mergers

2017 ◽  
Vol 13 (S338) ◽  
pp. 14-21
Author(s):  
Youjun Lu ◽  
Liang Cao ◽  
Yuetong Zhao
Keyword(s):  
Black Hole ◽  
Galaxy Formation ◽  
Stellar Mass ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Binary Black Holes ◽  
Massive Galaxies ◽  
Binary Black Hole ◽  
Hubble Time

AbstractWe report our investigations on the host galaxy properties of stellar binary black holes (SBBHs) by implementing simple recipes for SBBH formation and merger into cosmological galaxy formation model. If the time delay between SBBH formation and merger ranges from Gyr to the Hubble time, SBBH mergers at redshift z < 0.3 occur preferentially in big galaxies with stellar mass M* > 2 × 1010M⊙ and metallicities Z peaking around ~0.6Z⊙. However, the host galaxy stellar mass distribution of heavy SBBH mergers (with total black hole mass >50M⊙) is bimodal with one peak at ~109M⊙ and the other peak at ~2 × 1010M⊙. The contribution fraction from metal-poor host galaxies (Z < 0.2Z⊙) to heavy mergers is much larger than that to less heavy mergers. If SBBHs were formed in the early universe, their mergers detected at z < 0.3 occur preferentially in even more massive galaxies with M* > 3 × 1010M⊙ and in galaxies with metallicities mostly >0.2Z⊙ and peaking at Z ~ 0.6Z⊙.

scholarly journals The Black Hole Mass of BL Lacertae Objects from the Stellar Velocity Dispersion of the Host Galaxy

2002 ◽  
Vol 569 (1) ◽  
pp. L35-L38 ◽  
Author(s):  
R. Falomo ◽  
J. K. Kotilainen ◽  
A. Treves
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Bl Lacertae Objects ◽  
Bl Lacertae ◽  
Stellar Velocity
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