The globular cluster/central black hole connection in galaxies

Harris, G. L. H.; Harris, William E.

doi:10.1111/j.1365-2966.2010.17606.x

Cited by 46 publications

(21 citation statements)

References 79 publications

(102 reference statements)

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“…Most influential was the discovery of a tight correlation between M • and the velocity dispersion σ of the host bulge at radii where stars mainly feel each other and not the BH (Ferrarese & Merritt 2000;Gebhardt et al 2000;Tremaine et al 2002;Gültekin et al 2009). Correlations are also observed between M • and bulge luminosity (Kormendy 1993a;Kormendy & Richstone 1995;Magorrian et al 1998), bulge mass (Dressler 1989;McLure & Dunlop 2002;Marconi & Hunt 2003;Häring & Rix 2004;); core parameters of elliptical galaxies (Milosavljević et al 2002;Ravindranath et al 2002;Graham 2004;Ferrarese et al 2006;Merritt 2006;Lauer et al 2007;), and globular cluster content (Burkert & Tremaine 2010;Harris & Harris 2011). These have led to the belief that BHs and bulges coevolve and regulate each other's growth (e. g., Silk & Rees 1998;Richstone et al 1998;Granato et al 2004;Di Matteo et al 2005;Springel et al 2005;Hopkins et al 2006;Somerville et al 2008).…”

Section: Supermassive Black Holes Do Not Correlate With Pseudobulgesmentioning

confidence: 98%

Secular evolution in disk galaxies

Kormendy¹

2013

Secular Evolution of Galaxies

124

138

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Self-gravitating systems evolve toward the most tightly bound configuration that is reachable via the evolution processes that are available to them. They do this by spreading -the inner parts shrink while the outer parts expand -provided that some physical process efficiently transports energy or angular momentum outward. The reason is that self-gravitating systems have negative specific heats. As a result, the evolution of stars, star clusters, protostellar and protoplanetary disks, black hole accretion disks and galaxy disks are fundamentally similar. How evolution proceeds then depends on the evolution processes that are available to each kind of self-gravitating system. These processes and their consequences for galaxy disks are the subjects of my lectures and of this Canary Islands Winter School.I begin with a review of the formation, growth and death of bars. Then I review the slow ("secular") rearrangement of energy, angular momentum, and mass that results from interactions between stars or gas clouds and collective phenomena such as bars, oval disks, spiral structure and triaxial dark halos. The "existence-proof" phase of this work is largely over: we have a good heuristic understanding of how nonaxisymmetric structures rearrange disk gas into outer rings, inner rings and stuff dumped onto the center. The results of simulations correspond closely to the morphology of barred and oval galaxies. Gas that is transported to small radii reaches high densities. Observations confirm that many barred and oval galaxies have dense central concentrations of gas and star formation. The result is to grow, on timescales of a few Gyr, dense central components that are frequently mistaken for classical (elliptical-galaxy-like) bulges but that were grown slowly out of the disk (not made rapidly by major mergers). The resulting picture of secular galaxy evolution accounts for the richness observed in galaxy structure.

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Section: Supermassive Black Holes Do Not Correlate With Pseudobulgesmentioning

confidence: 98%

Secular evolution in disk galaxies

Kormendy¹

2013

Secular Evolution of Galaxies

124

138

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“…One could at least constrain well-defined models of cluster formation. If GC-formation was triggered by galactic scale shock waves (Harris & Harris 2011), e.g. associated with galactic winds and jets (Krause 2002(Krause , 2005a, where the GCs are supposed to form in a galactic wind shell, one might expect some active GCs during the time when the jet is active too, thus marking the relevant evolutionary epoch of the GCs.…”

Section: Gas Expulsion Powered By Dark-remnant Accretion and Possiblementioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause¹,

Charbonnel²,

Decressin³

et al. 2012

A&A

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The picture of the early evolution of globular clusters has been significantly revised in recent years. Current scenarios require at least two generations of stars of which the first generation (1G), and therefore also the protocluster cloud, has been much more massive than the currently predominating second generation (2G). Fast gas expulsion is thought to unbind the majority of the 1G stars. Gas expulsion is also mandatory to remove metal-enriched supernova ejecta, which are not found in the 2G stars. It has long been thought that the supernovae themselves are the agent of the gas expulsion, based on crude energetics arguments. Here, we assume that gas expulsion happens via the formation of a superbubble, and describe the kinematics by a thin-shell model. We find that supernovadriven shells are destroyed by the Rayleigh-Taylor instability before they reach escape speed for all but perhaps the least massive and most extended clusters. More power is required to expel the gas, which might plausibly be provided by a coherent onset of accretion onto the stellar remnants. The resulting kpc-sized bubbles might be observable in Faraday rotation maps with the planned Square Kilometre Array radio telescope against polarised background radio lobes if a globular cluster would happen to form in front of such a radio lobe.

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“…This is so far unclear, and different scenarios are considered (compare e.g. Harris et al 1998;Krause 2002;Kravtsov & Gnedin 2005;Gnedin 2011;Gray & Scannapieco 2011;Harris & Harris 2011). In general, one may consider two classes of physical conditions: First, the first-generation stars could be formed while the gas is in free collapse.…”

Section: Support Of the Gas And Relation To Gc Formation Scenariosmentioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause

Charbonnel

Decressin

et al. 2013

A&A

139

155

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Context. The self-enrichment scenario for globular clusters (GC) requires large amounts of residual gas after the initial formation of the first stellar generation. Recently, we found that supernovae may not be able to expel that gas, as required to explain their presentday gas-free state, and suggested that a sudden accretion onto the dark remnants at a stage when type II supernovae have ceased may plausibly lead to fast gas expulsion. Aims. Here, we explore the consequences of these results for the self-enrichment scenario via fast-rotating massive stars (FRMS). Methods. We analysed the interaction of FRMS with the intra-cluster medium (ICM), in particular where, when, and how the second generation of stars may form. From the results, we developed a timeline of the first ≈40 Myr of GC evolution. Results. Our previous results imply three phases during which the ICM is in a fundamentally different state, namely the wind bubble phase (lasting 3.5 to 8.8 Myr), the supernova phase (lasting 26.2 to 31.5 Myr), and the dark remnant accretion phase (lasting 0.1 to 4 Myr): (i) Quickly after the first-generation massive stars have formed, stellar wind bubbles compress the ICM into thin filaments. No stars may form in the normal way during this phase because of the high Lyman-Werner flux density. If the first-generation massive stars have equatorial ejections however, as we proposed in the FRMS scenario, accretion may resume in the shadow of the equatorial ejecta. The second-generation stars may then form due to gravitational instability in these disc, which are fed by both the FRMS ejecta and pristine gas. (ii) In the supernova phase the ICM develops strong turbulence, with characteristic velocities below the escape velocity. The gas does not accrete either onto the stars or onto the dark remnants in this phase because of the high gas velocities. The strong mass loss associated with the transformation of the FRMS into dark remnants then leads to the removal of the secondgeneration stars from the immediate vicinity of the dark remnants. (iii) When the supernovae have ceased, turbulence quickly decays, and the gas can once more accrete, now onto the dark remnants. As discussed previously, this may release sufficient energy to unbind the gas, and may happen fast enough so that a large fraction of less tightly bound first-generation stars are lost. Conclusions. Studying the FRMS scenario for the self-enrichment of GCs in detail reveals the important role of the physics of the ICM for our understanding of the formation and early evolution of GCs. Depending on the level of mass segregation, this sets constraints on the orbital properties of the stars, in particular high orbital eccentricities, which likely has implications on the GC formation scenario.

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The globular cluster/central black hole connection in galaxies

Cited by 46 publications

References 79 publications

Secular evolution in disk galaxies

Secular evolution in disk galaxies

Superbubble dynamics in globular cluster infancy

Superbubble dynamics in globular cluster infancy

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