Star cluster dynamics

Vesperini, Enrico

doi:10.1098/rsta.2009.0260

Cited by 26 publications

(23 citation statements)

References 171 publications

(286 reference statements)

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“…The total mass in the GCS has been continually decreasing since their formation epoch; during the first several ∼10 7 yr of a young massive star cluster's life, it sheds a high fraction of its initial protocluster gas due to SNe and stellar winds, and the highest mass stars evolve and disappear. Over the subsequent Hubble time, tidal stripping and evaporation remove most low‐mass clusters, and the higher mass ones are significantly eroded (see Vesperini 2010, for a review). These factors combined mean that the initial mass in the GC system should have been many times larger than it is now.…”

Section: Discussionmentioning

confidence: 99%

The globular cluster/central black hole connection in galaxies

Harris¹,

Harris²

2010

Monthly Notices of the Royal Astronomical Society

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We explore the relation between the total globular population in a galaxy (NGC) and the mass of its central black hole (M•). Using a sample of 33 galaxies, twice as large as the original sample discussed by Burkert & Tremaine (2010), we find that NGC for elliptical and spiral galaxies increases in almost precisely direct proportion to M•. The S0‐type galaxies by contrast do not follow a clear trend, showing large scatter in M• at a given NGC. After accounting for observational measurement uncertainty, we find that the mean relation defined by the E and S galaxies must also have an intrinsic or ‘cosmic’ scatter of ±0.2 in either log NGC or log M•. The residuals from this correlation show no trend with globular cluster specific frequency. We suggest that these two types of galaxy subsystems (central black hole and globular cluster system) may be closely correlated because they both originated at high redshift during the main epoch of hierarchical merging, and both require extremely high‐density conditions for formation. Lastly, we note that roughly 10 per cent of the galaxies in our sample (one E, one S and two S0) deviate strongly from the main trend, all in the sense that their M• is at least 10 times smaller than would be predicted by the mean relation.

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Section: Discussionmentioning

confidence: 99%

The globular cluster/central black hole connection in galaxies

Harris¹,

Harris²

2010

Monthly Notices of the Royal Astronomical Society

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“…Harris et al additionally determine MGCS for each galaxy in their catalog. Harris et al determine the total GC V-band luminosity in each galaxy using the galaxies' V-band magnitudes and the GC luminosity function described in Jordan et al (2006) and Vesperini (2010). To derive MGCS, they then scale total GC luminosity to total GC mass using a mass-tolight ratio of 2.…”

Section: Globular Cluster Photometric Datamentioning

confidence: 99%

Revisiting the X-ray – Mass scaling relations of early-type galaxies with the mass of their globular cluster systems as a proxy for the total galaxy mass

Kim

James

Fabbiano

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using globular cluster (GC) kinematics and photometry data, we calibrate the scaling relation between the total galaxy mass (MTOT including dark matter) and total globular cluster system mass (MGCS) in a sample of 30 early-type galaxies (ETG), confirming a nearly linear relationship between the two physical parameters. Using samples of 83 and 57 ETGs, we investigate this scaling relation in conjunction with the previously known relations between MTOT and the ISM Xray luminosity and temperature, respectively. We confirm that MGCS can be effectively used as a proxy of MTOT. We further find that the LX,GAS -MTOT relation is far tighter in the subsample of core ETGs, when compared to cusp ETGs. In core ETGs (old, passively evolving stellar systems) MTOT is significantly larger than the total stellar mass MSTAR and the correlation with the hot gas properties is driven by their dark matter mass MDM. Cusp ETGs have typically lower LX,GAS than core ETGs. In cusp ETGs, for a given MDM, higher LX,GAS is associated with higher MSTAR, suggesting stellar feedback as an important secondary factor for heating the ISM. Using the MGCS-MTOT scaling relations we compare 272 ETGs with previous estimates of the stellar-to-halo mass relation of galaxies. Our model-independent estimate of MTOT results in a good agreement around halo masses of 10 12 M, but suggest higher star formation efficiency than usually assumed both at the low and at the high halo mass ends.

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“…The focus being on the link between the clusters and their galactic and cosmological context, it does not address the topics of internal cluster physics and their stellar populations in details, nor the state of the art on the observational side of the subject. I encourage the reader to explore complementary reviews on these topics, in particular in • Naab and Ostriker (2017): galaxy formation • Portegies Zwart et al (2010) and Adamo and Bastian (2015): young massive clusters • Heggie and Hut (2003) and Vesperini (2010): internal dynamics of clusters • Aarseth (2003): N-body simulations of clusters.…”

Section: Evolution 21mentioning

confidence: 99%

“…The simplest and historical approach accounting for this consists in considering clusters on fixed circular or elliptical orbits in an analytical representation of the galactic potential, where the tidal force can be expressed analytically and added to the force every star experiences from the rest of the cluster (e.g. Weinberg 1990 andOstriker 1997 with the Fokker-Planck method, Vesperini andPortegies Zwart et al 1998 with the N-body way, and Giersz 2001 with the Monte Carlo approach). To go further, the galactic potential can also be used to integrate the orbit of the cluster and compute the relevant tidal forces, thus allowing for non-fixed orbits (Renaud and Gieles, 2015a).…”

Section: Accounting For the Environmentmentioning

confidence: 99%

Star clusters in evolving galaxies

Renaud

2018

New Astronomy Reviews

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Their ubiquity and extreme densities make star clusters probes of prime importance of galaxy evolution. Old globular clusters keep imprints of the physical conditions of their assembly in the early Universe, and younger stellar objects, observationally resolved, tell us about the mechanisms at stake in their formation. Yet, we still do not understand the diversity involved: why is star cluster formation limited to 10 5 M objects in the Milky Way, while some dwarf galaxies like NGC 1705 are able to produce clusters 10 times more massive? Why do dwarfs generally host a higher specific frequency of clusters than larger galaxies? How to connect the present-day, often resolved, stellar systems to the formation of globular clusters at high redshift? And how do these links depend on the galactic and cosmological environments of these clusters? In this review, I present recent advances on star cluster formation and evolution, in galactic and cosmological context. The emphasis is put on the theory, formation scenarios and the effects of the environment on the evolution of the global properties of clusters. A few open questions are identified.

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Star cluster dynamics

Cited by 26 publications

References 171 publications

The globular cluster/central black hole connection in galaxies

The globular cluster/central black hole connection in galaxies

Revisiting the X-ray – Mass scaling relations of early-type galaxies with the mass of their globular cluster systems as a proxy for the total galaxy mass

Star clusters in evolving galaxies

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