scholarly journals The formation of bulges and black holes: lessons from a census of active galaxies in the SDSS

2005 ◽  
Vol 363 (1828) ◽  
pp. 621-643 ◽  
Author(s):  
Guinevere Kauffmann ◽  
Timothy M. Heckman
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Emission Line ◽  
Time Scale ◽  
Mass Scale ◽  
Growth Time ◽  
Normal Galaxies ◽  
Black Hole Accretion ◽  
Order Of Magnitude ◽  
Hole Accretion

We examine the relationship between galaxies, supermassive black holes and AGN using a sample of 23 000 narrow–emission–line (‘type 2’) active galactic nuclei (AGN) drawn from a sample of 123 000 galaxies from the Sloan Digital Sky Survey. We have studied how AGN host properties compare with those of normal galaxies and how they depend on the luminosity of the active nucleus. We find that AGN reside in massive galaxies and have distributions of sizes and concentrations that are similar to those of the early–type galaxies in our sample. The host galaxies of low–luminosity AGN have stellar populations similar to normal early types. The hosts of highluminosity AGN have much younger mean stellar ages, and a significant fraction have experienced recent starbursts. High–luminosity AGN are also found in lower–density environments. We then use the stellar velocity dispersions of the AGN hosts to estimate black hole masses and their [OIII]λ5007 emission–line luminosities to estimate black hole accretion rates.We find that the volume averaged ratio of star formation to black hole accretion is ∼1000 for the bulge–dominated galaxies in our sample. This is remarkably similar to the observed ratio of stellar mass to black hole mass in nearby bulges. Most of the present–day black hole growth is occurring in black holes with masses less than 3 × 10 7 M ⊙. Our estimated accretion rates imply that low–mass black holes are growing on a time–scale that is comparable with the age of the Universe. Around 50% this growth takes place in AGN that are radiating within a factor of five of the Eddington luminosity. Such systems are rare, making up only 0.2% of the lowmass black hole population at the present day. The remaining growth occurs in lower luminosity AGN. The growth time–scale increases by more than an order of magnitude for the most massive black holes in our sample. We conclude that the evolution of the AGN luminosity function documented in recent optical and X–ray surveys is driven by a decrease in the characteristic mass scale of actively accreting black holes.

scholarly journals Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

2019 ◽  
Vol 493 (1) ◽  
pp. 1500-1511 ◽  
Author(s):  
Francesco Shankar ◽  
David H Weinberg ◽  
Christopher Marsden ◽  
Philip J Grylls ◽  
Mariangela Bernardi ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Selection Bias ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Independent Evidence ◽  
X Ray ◽  
Black Hole Accretion ◽  
Black Hole Masses ◽  
Hole Accretion

ABSTRACT The masses of supermassive black holes at the centres of local galaxies appear to be tightly correlated with the mass and velocity dispersions of their galactic hosts. However, the local Mbh–Mstar relation inferred from dynamically measured inactive black holes is up to an order-of-magnitude higher than some estimates from active black holes, and recent work suggests that this discrepancy arises from selection bias on the sample of dynamical black hole mass measurements. In this work, we combine X-ray measurements of the mean black hole accretion luminosity as a function of stellar mass and redshift with empirical models of galaxy stellar mass growth, integrating over time to predict the evolving Mbh–Mstar relation. The implied relation is nearly independent of redshift, indicating that stellar and black hole masses grow, on average, at similar rates. Matching the de-biased local Mbh–Mstar relation requires a mean radiative efficiency ε ≳ 0.15, in line with theoretical expectations for accretion on to spinning black holes. However, matching the ‘raw’ observed relation for inactive black holes requires ε ∼ 0.02, far below theoretical expectations. This result provides independent evidence for selection bias in dynamically estimated black hole masses, a conclusion that is robust to uncertainties in bolometric corrections, obscured active black hole fractions, and kinetic accretion efficiency. For our fiducial assumptions, they favour moderate-to-rapid spins of typical supermassive black holes, to achieve ε ∼ 0.12–0.20. Our approach has similarities to the classic Soltan analysis, but by using galaxy-based data instead of integrated quantities we are able to focus on regimes where observational uncertainties are minimized.

scholarly journals Transonic structure of slowly rotating accretion flows with shocks around black holes

2016 ◽  
Vol 12 (S324) ◽  
pp. 23-26
Author(s):  
Petra Suková ◽  
Szymon Charzyński ◽  
Agnieszka Janiuk
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Time Scale ◽  
Mass Scale ◽  
Schwarzschild Black Hole ◽  
Transonic Flows ◽  
Accretion Flows ◽  
2D Structure ◽  
Sgr A

AbstractWe present recent results of the studies of low angular momentum accretion of matter onto Schwarzschild black hole using fully relativistic numerical simulations. We compare the resulting 2D structure of transonic flows with results of 1D pseudo-Newtonian computations of non-magnetized flow. The research has observable consequences on black holes on the whole mass scale, in particular it is related to the time-scale and shape of luminosity flares in Sgr A* or to the evolution of QPO frequency during outbursts of microquasars.

scholarly journals X-ray reflection spectroscopy with Kaluza–Klein black holes

2020 ◽  
Vol 80 (7) ◽  
Author(s):  
Jiachen Zhu ◽  
Askar B. Abdikamalov ◽  
Dimitry Ayzenberg ◽  
Mustapha Azreg-Aïnou ◽  
Cosimo Bambi ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Alternative Theory ◽  
Disk System ◽  
X Ray ◽  
Black Hole Accretion ◽  
Klein Theory ◽  
Black Hole Accretion Disk ◽  
Hole Accretion ◽  
Kaluza Klein

Abstract Kaluza–Klein theory is a popular alternative theory of gravity, with both non-rotating and rotating black hole solutions known. This allows for the possibility that the theory could be observationally tested. We present a model which calculates the reflection spectrum of a black hole accretion disk system, where the black hole is described by a rotating solution of the Kaluza–Klein theory. We also use this model to analyze X-ray data from the stella-mass black hole in GRS 1915+105 and provide constraints on the free parameters of the Kaluza–Klein black holes.

scholarly journals Finite gravitational time dilation in black holes using dynamic Newtonian advanced gravity (DNAg)

2016 ◽  
Vol 94 (3) ◽  
pp. 279-282
Author(s):  
Andrew Worsley ◽  
Joseph Worsley
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Time Dilation ◽  
Newtonian Gravity ◽  
Navigation Systems ◽  
Black Hole Accretion ◽  
Dynamic Form ◽  
Satellite Navigation Systems ◽  
Gravitational Equations ◽  
Hole Accretion

In this paper we use a dynamic form of modified Newtonian gravity to reformulate the equations for gravitational time dilation. Here we introduce the generic equations for gravitational time dilation. It is shown that these equations agree exactly with gravitational time dilation in satellite navigation systems. The equations are also in agreement with a reanalysis of observations of gravitational red shifts in black hole accretion discs. Using these equations, we translate the time dilation into a finite value at the black hole event horizon. Thus this reformulation resolves the difficulties of the existence of black hole singularities. Importantly these dynamic gravitational equations provide testable predictions in the vicinity of black holes.

scholarly journals Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

2020 ◽  
Vol 642 ◽  
pp. A65
Author(s):  
R. Carraro ◽  
G. Rodighiero ◽  
P. Cassata ◽  
M. Brusa ◽  
F. Shankar ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Star Formation ◽  
Stellar Mass ◽  
Starburst Galaxies ◽  
Black Hole Mass ◽  
X Ray ◽  
Star Forming ◽  
Black Hole Accretion ◽  
Hole Accretion

Aims. We study the coevolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different phases of galaxy life: main-sequence star-forming galaxies, quiescent galaxies, and starburst galaxies at different cosmic epochs. Methods. We exploited the unique combination of depth and area in the COSMOS field and took advantage of the X-ray data from the Chandra COSMOS-Legacy survey and the extensive multiwavelength ancillary data presented in the COSMOS2015 catalog, including in particular the UVista Ultra-deep observations. These large datasets allowed us to perform an X-ray stacking analysis and combine it with detected sources in a broad redshift interval (0.1 <  z <  3.5) with unprecedented statistics for normal star-forming, quiescent, and starburst galaxies. The X-ray luminosity was used to predict the black holeAR, and a similar stacking analysis on far-infrared Herschel maps was used to measure the corresponding obscured SFR for statistical samples of sources in different redshifts and stellar mass bins. Results. We focus on the evolution of the average SFR-stellar mass (M*) relation and compare it with the BHAR-M* relation. This extends previous works that pointed toward the existence of almost linear correlations in both cases. We find that the ratio between BHAR and SFR does not evolve with redshift, although it depends on stellar mass. For the star-forming populations, this dependence on M* has a logarithmic slope of ∼0.6 and for the starburst sample, the slope is ∼0.4. These slopes are both at odds with quiescent sources, where the dependence remains constant (log(BHAR/SFR) ∼ −3.4). By studying the specific BHAR and specific SFR, we find signs of downsizing for M* and black hole mass (MBH) in galaxies in all evolutionary phases. The increase in black hole mass-doubling timescale was particularly fast for quiescents, whose super-massive black holes grew at very early times, while accretion in star-forming and starburst galaxies continued until more recent times. Conclusions. Our results support the idea that the same physical processes feed and sustain star formation and black hole accretion in star-forming galaxies while the starburst phase plays a lesser role in driving the growth of the supermassive black holes, especially at high redshift. Our integrated estimates of the M* − MBH relation at all redshifts are consistent with independent determinations of the local M* − MBH relation for samples of active galactic nuclei. This adds key evidence that the evolution in the BHAR/SFR is weak and its normalization is relatively lower than that of local dynamical M* − MBH relations.

scholarly journals The most massive black holes on the Fundamental Plane of black hole accretion

2017 ◽  
Vol 474 (1) ◽  
pp. 1342-1360 ◽  
Author(s):  
M. Mezcua ◽  
J. Hlavacek-Larrondo ◽  
J. R. Lucey ◽  
M. T. Hogan ◽  
A. C. Edge ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Fundamental Plane ◽  
Massive Black Holes ◽  
Black Hole Accretion ◽  
Hole Accretion

scholarly journals Reionization with galaxies and active galactic nuclei

2020 ◽  
Vol 495 (3) ◽  
pp. 3065-3078 ◽  
Author(s):  
Pratika Dayal ◽  
Marta Volonteri ◽  
Tirthankar Roy Choudhury ◽  
Raffaella Schneider ◽  
Maxime Trebitsch ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Star Formation ◽  
High Redshift ◽  
Mass Function ◽  
Stellar Mass ◽  
Relative Role ◽  
Black Hole Accretion ◽  
Wide Range ◽  
Hole Accretion

ABSTRACT In this work we investigate the properties of the sources that reionized the intergalactic medium (IGM) in the high-redshift Universe. Using a semi-analytical model aimed at reproducing galaxies and black holes in the first ∼1.5 Gyr of the Universe, we revisit the relative role of star formation and black hole accretion in producing ionizing photons that can escape into the IGM. Both star formation and black hole accretion are regulated by supernova feedback, resulting in black hole accretion being stunted in low-mass haloes. We explore a wide range of combinations for the escape fraction of ionizing photons (redshift-dependent, constant, and scaling with stellar mass) from both star formation ($\langle f_{\rm esc}^{\rm sf} \rangle$) and AGN ($f_{\rm esc}^{\rm bh}$) to find: (i) the ionizing budget is dominated by stellar radiation from low stellar mass ($M_*\lt 10^9 \, {\rm \rm M_\odot }$) galaxies at z &gt; 6 with the AGN contribution (driven by $M_{bh}\gt 10^6 \, {\rm \rm M_\odot }$ black holes in $M_* \gtrsim 10^9\, {\rm \rm M_\odot }$ galaxies) dominating at lower redshifts; (ii) AGN only contribute $10-25{{\ \rm per\ cent}}$ to the cumulative ionizing emissivity by z = 4 for the models that match the observed reionization constraints; (iii) if the stellar mass dependence of $\langle f_{\rm esc}^{\rm sf} \rangle$ is shallower than $f_{\rm esc}^{\rm bh}$, at z &lt; 7 a transition stellar mass exists above which AGN dominate the escaping ionizing photon production rate; (iv) the transition stellar mass decreases with decreasing redshift. While AGN dominate the escaping emissivity above the knee of the stellar mass function at z ∼ 6.8, they take-over at stellar masses that are a tenth of the knee mass by z = 4.

scholarly journals Population Synthesis of GRB Progenitors: Problems With Kicks

2000 ◽  
Vol 195 ◽  
pp. 339-346
Author(s):  
C. L. Fryer
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Stars ◽  
Accretion Disks ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Population Synthesis ◽  
Black Hole Accretion ◽  
Black Hole Accretion Disk ◽  
Hole Accretion

Accretion disks around stellar-mass black holes are now thought to be the engines which power classical gamma-ray bursts (GRBs). These disks are formed almost exclusively in binaries, and to study the characteristics of the progenitors of these black-hole accretion disk (BHAD) GRBs, we must understand the uncertainties in binary population synthesis calculations. Kicks imparted onto nascent neutron stars and black holes are among the most misunderstood concepts of binary population synthesis. In this paper, we outline the current understanding (or lack of understanding) of these kicks and discuss their effect on BHAD GRBs and binary population synthesis as a whole.

scholarly journals Mechanical feedback effects on primordial black hole accretion

2020 ◽  
Vol 638 ◽  
pp. A132 ◽  
Author(s):  
V. Bosch-Ramon ◽  
N. Bellomo
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Accretion Rate ◽  
Compact Object ◽  
Primordial Black Hole ◽  
Primordial Black Holes ◽  
Black Hole Accretion ◽  
The Impact ◽  
Hole Accretion ◽  
Mechanical Feedback

Context. Dark matter may consist, at least partially, of primordial black holes formed during the radiation-dominated era. The radiation produced by accretion onto primordial black holes leaves characteristic signatures on the properties of the medium at high redshift, before and after hydrogen recombination. Therefore, reliable modeling of accretion onto these objects is required to obtain robust constraints on their abundance. Aims. We investigate the effect of mechanical feedback, that is, the impact of outflows (winds and– or –jets) on the medium, on primordial black hole accretion, and thereby on the associated radiation. Methods. Using analytical and numerical calculations, we studied for the first time the possibility that outflows can reduce the accretion rate of primordial black holes with masses similar to those detected by the LIGO-Virgo collaboration. Results. Despite the complexity of the accretion rate evolution, mechanical feedback is useful in to significantly reducing the primordial black hole accretion rate, at least by one order of magnitude, when outflows are aligned with the motion of the compact object. If the outflow is perpendicular to the direction of motion, the effect is less important, but it is still non-negligible. Conclusions. Outflows from primordial black holes, even rather weak ones, can significantly decrease the accretion rate, effectively weakening abundance constraints on these objects. Our results motivate further numerical simulations with a more realistic setup, which would yield more precise quantitative predictions.

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