Evolution of two stellar populations in globular clusters

Decressin, T.; Baumgardt, Holger; Charbonnel, C.; Kroupa, Pavel

doi:10.1051/0004-6361/200913703

Cited by 75 publications

(135 citation statements)

References 69 publications

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“…In addition, there should be a region in the parameter space in which all clusters will be totally disrupted. The outcome of our N -body simulations are consistent with Decressin et al (2010) who analysed the N -body models of Baumgardt & Kroupa (2007). As it is inferred from Fig.…”

Section: Resultssupporting

confidence: 91%

“…According to Fig. 5 of Decressin et al (2010) in a cluster with M = 10 6 M , at most 400 SNe/ Myr will explode within 1 Myr implying that only 40 SNe will go off in 10 5 yr which is a factor 3 to 6 below the required limit. As a result SN explosions seem not to able to generate enough energy to expel the gas over the short time-scales we need in our scenario.…”

Section: Conclusion and Discussionmentioning

confidence: 98%

“…According to Decressin et al (2010) for a gas cloud with an initial mass of ∼ 10 6 M and an initial half-mass radius of 0.5 pc, around 50 SNe are needed to unbind the gas cloud. In our case the gas clouds, which are more concentrated than the first generation stars, have initial half-mass radii of 0.1 and 0.2 pc.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

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Dynamical constraints on the origin of multiple stellar populations in globular clusters

Khalaj¹,

Baumgardt²

2015

Mon. Not. R. Astron. Soc.

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We have carried out a large grid of N -body simulations in order to investigate if massloss as a result of primordial gas expulsion can be responsible for the large fraction of second generation stars in globular clusters (GCs) with multiple stellar populations (MSPs). Our clusters start with two stellar populations in which 10% of all stars are second generation stars. We simulate clusters with different initial masses, different ratios of the half-mass radius of first to second generation stars, different primordial gas fractions and Galactic tidal fields with varying strength. We then let our clusters undergo primordial gas-loss and obtain their final properties such as mass, half-mass radius and the fraction of second generation stars. Using our N -body grid we then perform a Monte Carlo analysis to constrain the initial masses, radii and required gas expulsion time-scales of GCs with MSPs. Our results can explain the present-day properties of GCs only if (1) a substantial amount of gas was present in the clusters after the formation of second generation stars and (2) gas expulsion time-scales were extremely short ( 10 5 yr). Such short gas expulsion time-scales are in agreement with recent predictions that dark remnants have ejected the primordial gas from globular clusters, and pose a potential problem for the AGB scenario. In addition, our results predict a strong anti-correlation between the number ratio of second-generation stars in GCs and the present-day mass of GCs. So far, the observational data show only a significantly weaker anti-correlation, if any at all.

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Section: Resultssupporting

confidence: 91%

Section: Conclusion and Discussionmentioning

confidence: 98%

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Dynamical constraints on the origin of multiple stellar populations in globular clusters

Khalaj¹,

Baumgardt²

2015

Mon. Not. R. Astron. Soc.

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“…These aspects outline another key difference between the AGB and FRMS scenario, i.e. that in order to explain the different proportions and radial distributions of FG and SG stars, the latter has to postulate that the SG was formed close to the massive stars in a mass-segregated star cluster (Decressin et al 2010).…”

Section: Proto-globular Clustersmentioning

confidence: 99%

Paving the way for the JWST: witnessing globular cluster formation at z > 3

Vanzella¹,

Calura²,

Meneghetti³

et al. 2017

Monthly Notices of the Royal Astronomical Society

180

215

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We report on five compact, extremely young (< 10 Myr) and blue (β U V < −2.5, F λ = λ β ) objects observed with VLT/MUSE at redshift 3.1169, 3.235, in addition to three objects at z = 6.145. These sources are magnified by the Hubble Frontier Field galaxy clusters MACS J0416 and AS1063. Their de-lensed half light radii (R e ) are between 16 to 140 pc, the stellar masses are 1 − 20 × 10 6 M , the magnitudes are m U V = 28.8 − 31.4 (−17 < M U V < −15) and specific star formation rates can be as large as ∼ 800 Gyr −1 . Multiple images of these systems are widely separated in the sky (up to 50 ) and individually magnified by factors 3-40. Remarkably, the inferred physical properties of two objects are similar to those expected in some globular cluster formation scenarios, representing the best candidate proto-globular clusters (proto-GC) discovered so far. Rest-frame optical high dispersion spectroscopy of one of them at z = 3.1169 yields a velocity dispersion σ v 20 km s −1 , implying a dynamical mass dominated by the stellar mass. Another object at z = 6.145, with de-lensed31.4), shows a stellar mass and a star-formation rate surface density consistent with the values expected from popular GC formation scenarios. An additional star-forming region at z = 6.145, with de-lensed m U V 32, a stellar mass of 0.5 ×10 6 M and a star formation rate of 0.06 M yr −1 is also identified. These objects currently represent the faintest spectroscopically confirmed star-forming systems at z > 3, elusive even in the deepest blank fields. We discuss how proto-GCs might contribute to the ionization budget of the universe and augment Lyα visibility during reionization. This work underlines the crucial role of JWST in characterizing the restframe optical and near-infrared properties of such low-luminosity high−z objects.

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“…Following other recent work (e.g. Baumgardt et al 2008;Decressin et al 2010), we use a Plummer model for the spatial distribution of gas and stars. The gas mass inside a radius r is then given by…”

Section: The Thin-shell Modelmentioning

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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Evolution of two stellar populations in globular clusters

Cited by 75 publications

References 69 publications

Dynamical constraints on the origin of multiple stellar populations in globular clusters

Dynamical constraints on the origin of multiple stellar populations in globular clusters

Paving the way for the JWST: witnessing globular cluster formation at z > 3

Superbubble dynamics in globular cluster infancy

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