The connection between the formation of galaxies and that of their central supermassive black holes

2005 ◽  
Vol 363 (1828) ◽  
pp. 705-713
Author(s):  
Martin G. Haehnelt
Keyword(s):  
Black Holes ◽  
Dark Matter ◽  
Globular Clusters ◽  
Dwarf Galaxies ◽  
High Redshift ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
Essential Ingredient ◽  
Open Questions ◽  
Very High

Massive black holes appear to be an essential ingredient of massive galactic bulges but little is known yet to what extent massive black holes reside in dwarf galaxies and globular clusters. Massive black holes most likely grow by a mixture of merging and accretion of gas in their hierarchically merging host galaxies. While the hierarchical merging of dark matter structures extends to sub-galactic scales and very high redshift, it is uncertain if the same is true for the build–up of massive black holes. I discuss here some of the relevant problems and open questions.

scholarly journals AGN radiative feedback in the early growth of massive black holes

2019 ◽  
Vol 489 (4) ◽  
pp. 5225-5230
Author(s):  
W Ishibashi
Keyword(s):  
Black Holes ◽  
Early Universe ◽  
Radiation Pressure ◽  
Early Growth ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
Black Hole Growth ◽  
Hole Growth ◽  
The Impact ◽  
Very High

ABSTRACT Growing observational evidence confirms the existence of massive black holes ($M_{\rm BH} \sim 10^9 \, \mathrm{M}_{\odot }$), accreting at rates close to the Eddington limit, at very high redshifts ($z \gtrsim 6\!-\!7$) in the early Universe. Recent observations indicate that the host galaxies of the first quasars are chemically evolved systems, containing unexpectedly large amounts of dust. Such a combination of high luminosities and large dust content should form favourable physical conditions for radiative dusty feedback. We explore the impact of the active galactic nucleus (AGN) feedback, driven by radiation pressure on dust, on the early growth of massive black holes. Assuming Eddington-limited exponential black hole growth, we find that the dynamics and energetics of the radiation pressure-driven outflows also follow exponential trends at late times. We obtain modest outflow energetics (with momentum flux $\dot{p} \lesssim L/c$ and kinetic power $\dot{E}_{\rm k} \lesssim 10^{-3} L$), comparable with available observations of quasar-driven outflows at very high redshifts, but significantly lower than typically observed in local quasars and predicted by wind energy-driven models. AGN radiative dusty feedback may thus play an important role in powering galactic outflows in the first quasars in the early Universe.

scholarly journals Dwarf Galaxies with Optical Signatures of Accreting Massive Black Holes

2013 ◽  
Vol 9 (S304) ◽  
pp. 23-23
Author(s):  
Amy Reines ◽  
J. Greene ◽  
M. Geha
Keyword(s):  
Black Holes ◽  
Dwarf Galaxies ◽  
High Redshift ◽  
Formation Mechanisms ◽  
Seed Formation ◽  
Massive Black Holes ◽  
Massive Galaxies ◽  
Cosmological Context ◽  
Initial Seed ◽  
Stellar Masses

AbstractSupermassive black holes (BHs) live at the heart of essentially all massive galaxies with bulges, power AGN, and are thought to be important agents in the evolution of their hosts. Observations of high-redshift quasars demonstrate that supermassive BHs must start out with masses considerably in excess of normal stellar-mass BHs. However, we do not know how the initial “seed” BHs formed in the early Universe, how massive they were originally, or what types of galaxies they formed in. While direct observations of distant seed BHs and their hosts in the infant Universe are unobtainable with current capabilities, models of BH growth in a cosmological context indicate that present-day dwarf galaxies can place valuable constraints on seed masses and distinguish between various seed formation mechanisms at early times. Using optical spectroscopy from the SDSS, we have systematically assembled the largest sample of dwarf galaxies hosting AGN to date. These dwarf galaxies have stellar masses comparable to the Magellanic Clouds and contain some of the least-massive supermassive BHs known. I will present results from this study and discuss our ongoing efforts to find additional examples of AGN in dwarfs and help constrain theories for the formation of the first seed BHs at high redshift.

Hunting for Globular Clusters in the early universe

2019 ◽  
Vol 14 (S351) ◽  
pp. 212-215
Author(s):  
Frederika Phipps ◽  
Sadegh Khochfar ◽  
Anna Lisa Varri
Keyword(s):  
Dark Matter ◽  
High Resolution ◽  
Globular Clusters ◽  
Dwarf Galaxies ◽  
High Redshift ◽  
Stellar Systems ◽  
Mass Relation ◽  
Cosmological Context ◽  
Low Mass ◽  
Stellar Density

AbstractSetting the formation of globular clusters (GCs) within a cosmological context and characterising the properties of proto-GCs at high redshift is currently a major challenge. In this work, we address that challenge by exploring a suit of high-resolution cosmological simulations from the First Billion Years (FiBY) project z at ⩾6 to investigate theoretical scenarios concerning the formation of old, low-mass stellar systems with a particular focus on GCs. Two distinct groups of objects are identified in the simulations. The first group of objects, with a high baryon fraction, we associate with proto-GCs. The second group, that exhibit a high stellar fraction, could be forming ultra-faint dwarf galaxies (UFDs). The objects with high baryon fraction are promising proto-GC candidates because they have little to no dark matter (DM), have number densities consistent with predictions from the literature, are very compact and have a high stellar density. We fit and also assess the redshift-zero globular system mass - halo mass relation and find it provides a reasonable fit to our proto-GC objects, indicating that this relation is likely set at formation.

scholarly journals High-redshift quasars and their host galaxies – I. Kinematical and dynamical properties and their tracers

2019 ◽  
Vol 488 (3) ◽  
pp. 4004-4022 ◽  
Author(s):  
Alessandro Lupi ◽  
Marta Volonteri ◽  
Roberto Decarli ◽  
Stefano Bovino ◽  
Joseph Silk ◽  
...  
Keyword(s):  
Observational Studies ◽  
Stellar Population ◽  
State Of The Art ◽  
High Redshift ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
The Galaxy ◽  
Dynamical Properties ◽  
Very High ◽  
Resolution Data

ABSTRACT Observations of high-redshift quasars provide information on the massive black holes (MBHs) powering them and the galaxies hosting them. Current observations of z ≳ 6 hosts, at sub-millimetre wavelengths, trace the properties of cold gas, and these are used to compare with the correlations between MBHs and galaxies characterizing the z = 0 population. The relations at z = 0, however, rely on stellar-based tracers of the galaxy properties. We perform a very high resolution cosmological zoom-in simulation of a z = 7 quasar including state-of-the-art non-equilibrium chemistry, MBH formation, growth, and feedback, to assess the evolution of the galaxy host and the central MBH, and compare the results with recent ALMA observations of high-redshift quasars. We measure both the stellar-based quantities used to establish the z = 0 correlations, as well as the gas-based quantities available in z ≳ 6 observations, adopting the same assumptions and techniques used in observational studies. The high-redshift studies argued that MBHs at high redshift deviate from the local MBH–galaxy correlations. In our analysis of the single galaxy we evolve, we find that the high-redshift population sits on the same correlations as the local one, when using the same tracers used at z = 0. When using the gas-based tracers, however, MBHs appear to be overmassive. The discrepancy between local and high-redshift MBHs seems to be caused by the different tracers employed, and the necessary assumptions, and not by an intrinsic difference. Better calibration of the tracers, higher resolution data, and availability of facilities that can probe the stellar population will be crucial to assess precisely and accurately high-redshift quasar hosts.

scholarly journals Voids in the Local Volume: a Limit on Appearance of a Galaxy in a Dark Matter Halo

2007 ◽  
Vol 3 (S244) ◽  
pp. 152-156
Author(s):  
Anton V. Tikhonov ◽  
Anatoly A. Klypin
Keyword(s):  
Dark Matter ◽  
High Resolution ◽  
Local Group ◽  
Dwarf Galaxies ◽  
Dark Matter Halo ◽  
Dark Matter Halos ◽  
Host Galaxies ◽  
Group Data ◽  
Luminous Matter ◽  
Very High

AbstractCurrent explanation of the overabundance of dark matter subhalos in the Local Group (LG) indicates that there maybe a limit on mass of a halo, which can host a galaxy. This idea can be tested using voids in the distribution of galaxies: at some level small voids should not contain any (even dwarf) galaxies. We use observational samples complete to MB = −12 with distances less than 8 Mpc to construct the void function (VF): the distribution of sizes of voids empty of any galaxies. There are ~ 30 voids with sizes ranging from 1 to 5 Mpc. We then study the distribution of dark matter halos in very high resolution simulations of the LCDM model. The theoretical VF matches the observations remarkably well only if we use halos with circular velocities larger than 45 ± 10 km/s. This agrees with the Local Group predictions. There are smaller halos in the voids, but they should not produce any luminous matter. Small voids look quite similar to their giant cousins: the density has a minimum at the center of a void and it increases as we get closer to the border. Small nonluminous halos inside the void form a web of tiny filaments. Thus, both the Local Group data and the nearby voids indicate that isolated halos below 45 ± 10 km/s must not host galaxies and that small (few Mpc) voids are truly dark.

scholarly journals Big and Young Supermassive Black Holes in the Early Universe

Galaxies ◽  
2021 ◽  
Vol 9 (2) ◽  
pp. 23
Author(s):  
Tullia Sbarrato
Keyword(s):  
Black Holes ◽  
Early Universe ◽  
Common Knowledge ◽  
Galactic Nuclei ◽  
Supermassive Black Holes ◽  
Massive Black Holes ◽  
Open Questions ◽  
Central Engine ◽  
Z Sources ◽  
Very High

Blazars are active galactic nuclei characterized by relativistic jets launched in the vicinity of the central engine (i.e., a supermassive black hole), which are oriented close to our line of sight. Their peculiar orientation makes them very efficient tracers of the overall jetted population, and due to their brightness they can be visible up to very high redshifts. A deep knowledge of these objects can provide fundamental clues to the models of formation and growth of the first supermassive black holes, but the search for them in the early Universe must be careful and follow a systematic approach. The discovery in the last ∼15 years of extremely massive blazars at very high redshifts (MBH>109M⊙, z>4) revolutionized our perception of their earliest evolution: there seem to be different formation epochs for extremely massive black holes hosted in jetted (z∼4) and non-jetted (z∼2.5) systems. This is not easy to explain, since one would expect jetted sources to accrete less efficiently. Small differences in the population are also derived from the search for such high-z sources. We will go through the open questions in order to understand where the common knowledge stands and which steps must be taken to better understand the formation and common evolution of supermassive black holes and jets in the early Universe.

scholarly journals Co-Evolution of Supermassive Black Holes and Their Host Galaxies

2009 ◽  
Vol 5 (S267) ◽  
pp. 34-39
Author(s):  
J. K. Kotilainen ◽  
R. Decarli ◽  
R. Falomo ◽  
A. Treves ◽  
M. Labita ◽  
...  
Keyword(s):  
Black Holes ◽  
Stellar Population ◽  
High Redshift ◽  
Host Galaxy ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
Galaxy Masses ◽  
Age Of The Universe ◽  
Black Hole Masses ◽  
The Universe

AbstractWe study the evolution of the MBH/Mhost relation up to z = 3 for a sample of 96 quasars with known host galaxy luminosities. Black hole masses are estimated assuming virial equilibrium in the broad-line regions, while the host galaxy masses are inferred from their luminosities. With this data, we are able to pin down the evolution of the MBH/Mhost relation over 85% of the age of the universe. While the MBH/Lhost relation remains nearly unchanged, taking into account the aging of the stellar population, we find that the MBH/Mhost ratio (Γ) increases by a factor ~ 7 from z = 0 to z = 3. We show that the evolution of Γ is independent of radio loudness and quasar luminosity. We propose that the most massive black holes, in their quasar phase at high-redshift, become extremely rare objects in host galaxies of similar mass in the local universe.

scholarly journals Observational Signatures of High-Redshift Quasars and Local Relics of Black Hole Seeds

2016 ◽  
Vol 33 ◽  
Author(s):  
Amy E. Reines ◽  
Andrea Comastri
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dwarf Galaxies ◽  
High Redshift ◽  
Observational Constraints ◽  
Solar Mass ◽  
Massive Black Holes ◽  
Eddington Limit ◽  
The Universe ◽  
Review Current

AbstractObservational constraints on the birth and early evolution of massive black holes come from two extreme regimes. At high redshift, quasars signal the rapid growth of billion-solar-mass black holes and indicate that these objects began remarkably heavy and/or accreted mass at rates above the Eddington limit. At low redshift, the smallest nuclear black holes known are found in dwarf galaxies and provide the most concrete limits on the mass of black hole seeds. Here, we review current observational work in these fields that together are critical for our understanding of the origin of massive black holes in the Universe.

scholarly journals Subhalo sinking and off-centre massive black holes in dwarf galaxies

2020 ◽  
Vol 495 (1) ◽  
pp. L12-L16 ◽  
Author(s):  
Pierre Boldrini ◽  
Roya Mohayaee ◽  
Joseph Silk
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dwarf Galaxies ◽  
Dynamical Friction ◽  
Host Galaxies ◽  
Transfer Energy ◽  
Massive Black Hole ◽  
Massive Black Holes ◽  
First Time

ABSTRACT Using fully GPU N-body simulations, we demonstrate for the first time that subhaloes sink and transfer energy via dynamical friction into the centres of dwarf galaxies. This dynamical heating kicks any central massive black hole out to tens of parsecs, especially at early epochs (z = 1.5–3). This mechanism helps explain the observed off-centre black holes (BHs) in dwarf galaxies and also predicts that off-centre BHs are more common in higher mass dwarf galaxies since dynamical friction becomes significantly weaker and BHs take more time to sink back towards the centres of their host galaxies. One consequence of off-centre BHs during early epochs of dwarf galaxies is to quench any BH feedback.

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