scholarly journals Mass to light ratios of Large Magellanic Cloud clusters

1991 ◽  
Vol 148 ◽  
pp. 191-192 ◽  
Author(s):  
Mario Mateo ◽  
Douglas Welch ◽  
Phil Fischer
Keyword(s):  
Globular Clusters ◽  
Massive Star ◽  
Large Range ◽  
Temporal Evolution ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Clusters ◽  
Large Numbers

The massive star clusters of the Large Magellanic Cloud (LMC) are ideal laboratories for the study of the dynamical evolution of rich stellar systems. Not only do they contain large numbers of stars but, unlike the Galactic globular clusters, LMC clusters span a large range in age. Here we describe a continuing project to determine the temporal evolution of the mass-to-light (M/L) ratio of LMC clusters and present some preliminary results.

scholarly journals Young star clusters in the LMC

1991 ◽  
Vol 148 ◽  
pp. 177-181
Author(s):  
K. C. Freeman ◽  
R.A.W. Elson
Keyword(s):  
Globular Clusters ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Large Magellanic Cloud ◽  
Young Star ◽  
Magellanic Cloud ◽  
Initial Mass ◽  
Young Star Clusters ◽  
Mass Functions

We discuss the integrated colours, kinematics, formation, dynamical evolution and initial mass functions of the young globular star clusters in the Large Magellanic Cloud (LMC). Because these clusters are so young, they offer us insights, unobtainable from the old globular clusters in our Galaxy, into the formation and early dynamical evolution of globular clusters.

scholarly journals Star clusters in the Magellanic Clouds

1991 ◽  
Vol 148 ◽  
pp. 161-164 ◽  
Author(s):  
S. van den Bergh
Keyword(s):  
Cluster Formation ◽  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Open Clusters ◽  
Small Magellanic Cloud ◽  
Cloud Clusters ◽  
The Galaxy

Star clusters in the Magellanic Clouds (MCs) differ from those in the Galaxy in a number of respects: (1) the Clouds contain a class of populous open clusters that has no Galactic counterpart; (2) Cloud clusters have systematically larger radii rh than those in the Galaxy; (3) clusters of all ages in the Clouds are, on average, more flattened than those in the Galaxy. In the Large Magellanic Cloud (LMC) there appear to have been two distinct epochs of cluster formation. LMC globulars have ages of 12-15 Gyr, whereas most populous open clusters have ages <5 Gyr. No such dichotomy is observed for clusters in the Small Magellanic Cloud (SMC) The fact that the SMC exhibits no enhanced cluster formation at times of bursts of cluster formation in the LMC, militates against encounters between the Clouds as a cause for enhanced rates of star and cluster formation.

scholarly journals Star clusters with dual red clumps

2009 ◽  
Vol 5 (S266) ◽  
pp. 320-325 ◽  
Author(s):  
Léo Girardi ◽  
Stefano Rubele ◽  
Leandro Kerber
Keyword(s):  
Composite Structures ◽  
Main Sequence ◽  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Sequence Evolution ◽  
Cloud Clusters ◽  
Red Clump ◽  
Secondary Feature ◽  
Single Cluster

AbstractA few star clusters in the Magellanic Clouds exhibit composite structures in the red-clump region of their colour–magnitude diagrams. The most striking case is NGC 419 in the Small Magellanic Cloud (SMC), where the red clump is composed of a main blob as well as a distinct secondary feature. This structure is demonstrated to be real and corresponds to the simultaneous presence of stars which passed through electron degeneracy after central-hydrogen exhaustion and those that did not. This rare occurrence in a single cluster allows us to set stringent constraints on its age and on the efficiency of convective-core overshooting during main-sequence evolution. We present a more detailed analysis of NGC 419, together with a first look at other populous Large Magellanic Cloud clusters which are apparently in the same phase: NGC 1751, NGC 1783, NGC 1806, NGC 1846, NGC 1852 and NGC 1917. We also compare these Magellanic Cloud cases with their Galactic counterparts, NGC 752 and NGC 7789. We emphasise the extraordinary potential of these clusters as absolute calibration marks on the age scale of stellar populations.

scholarly journals Observations of multiple populations in star clusters

2008 ◽  
Vol 4 (S258) ◽  
pp. 233-244 ◽  
Author(s):  
Giampaolo Piotto
Keyword(s):  
Globular Clusters ◽  
Star Clusters ◽  
Stellar Populations ◽  
Magellanic Cloud ◽  
Multiple Populations ◽  
Cloud Clusters ◽  
Photometric Observations ◽  
Galactic Globular Clusters

AbstractAn increasing number of photometric observations of multiple stellar populations in Galactic globular clusters is seriously challenging the paradigm of GCs hosting single, simple stellar populations. These multiple populations manifest themselves in a split of different evolutionary sequences as observed in the cluster color-magnitude diagrams. Multiple stellar populations have been identified in Galactic and Magellanic Cloud clusters. In this paper we will summarize the observational scenario.

Young, old, massive: Steps to understanding globular cluster formation

2019 ◽  
Vol 14 (S351) ◽  
pp. 3-12
Author(s):  
William E. Harris
Keyword(s):  
Galaxy Evolution ◽  
Globular Clusters ◽  
Massive Star ◽  
Cluster Formation ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Mass Range ◽  
High Mass ◽  
Theoretical Modelling ◽  
Giant Molecular Clouds

AbstractOn observational grounds we now know a huge amount about the characteristics of massive star clusters in galaxies of all types, from the smallest dwarfs to the most massive giants and even into the Intracluster Medium. The old globular clusters (GCs) in particular exhibit a high degree of uniformity across all these environments in their physical properties including scale size, luminosity distribution, metallicity distribution, and age. As survivors of a long period of dynamical evolution, they are “unusual, but not special” among star clusters.The past few years have seen major advances in theoretical modelling that are starting to reveal how these massive star clusters formed in the early stages of galaxy evolution. Several suites of models point to their emergence in GMCs (Giant Molecular Clouds), which provide the turbulent big reservoirs of gas within which star clusters can be built. At cluster masses ∼105M⊙ and above, clusters form hierarchically through a nearly equal combination of direct gas accretion, and mergers with smaller clusters scattered throughout the GMC. GCs and YMCs (young massive clusters) in this high mass range should therefore be composite systems right from birth. To make such high-mass clusters, host GMCs of ∼107M⊙ are needed, and these are most commonly found in galaxies at redshifts z ≳ 2.

scholarly journals Extended Surveys of MC Star Clusters

1994 ◽  
Vol 161 ◽  
pp. 497-501
Author(s):  
M. Kontizas ◽  
E. Kontizas
Keyword(s):  
Globular Clusters ◽  
Massive Star ◽  
Binary Star ◽  
Age Distribution ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Extended System ◽  
Dynamical Parameters ◽  
Stellar Associations ◽  
Early Phases

The location of the LMC clusters, their age distribution and dynamical parameters have shown that two star cluster systems exist in this galaxy: 1) one extended system, elliptical in shape, which contains all intermediate and old star clusters and 2) another system, again elliptical, but smaller in diameter, superimposed on the other and inclined by about 50 degrees from the latter. It contains the most massive, very young globular clusters which are still at their early phases of dynamical evolution. The existence of very rich stellar associations, binary star clusters and very elliptical ones located in this system, indicates that massive star clusters have formed very recently and are still under formation.

scholarly journals Metal abundances of Magellanic Cloud clusters

1991 ◽  
Vol 148 ◽  
pp. 341-342
Author(s):  
D. Geisler ◽  
A. McWilliam ◽  
N. Suntzeff ◽  
M. Mateo ◽  
J. Graham ◽  
...  
Keyword(s):  
Main Sequence ◽  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Small Sample ◽  
Magellanic Cloud ◽  
High Dispersion ◽  
Ccd Photometry ◽  
Elemental Abundances ◽  
Cloud Clusters ◽  
Metal Abundances

We have obtained Washington CCD photometry with the CTIO 4m and 1.5m for ˜50 intermediate-to-old age star clusters in the Clouds. The data extend to near or below the main sequence and provide excellent photometry for the giants, from which precise (internal errors <0.1 dex) mean cluster abundances can be determined. We present data for several of the clusters and discuss the results. Intermediate resolution spectra have also been obtained for some 16 clusters with the CTIO 4m ARGUS multiple-object fibre-fed spectrograph. Finally, we have also obtained high dispersion (R˜20,000) échelle spectra for several of the brighter giants in a small sample of Large Magellanic Cloud (LMC) clusters. Detailed elemental abundances derived from these spectra will be presented. These data will help refine our knowledge of the age-metallicity relation in the Clouds.

scholarly journals Young massive star clusters: achievements and challenges

2009 ◽  
Vol 5 (S266) ◽  
pp. 49-57 ◽  
Author(s):  
Richard de Grijs
Keyword(s):  
Massive Star ◽  
Initial Conditions ◽  
Cluster Formation ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Mass Function ◽  
Large Magellanic Cloud ◽  
Initial Mass Function ◽  
Ongoing Research ◽  
Mass Segregation

AbstractIn spite of significant recent and ongoing research efforts, most of the early evolution and long-term fate of young massive star clusters remain clouded in uncertainties. Here, I discuss our understanding of the initial conditions of star cluster formation and the importance of initial substructure for the subsequent dynamical-evolution and mass-segregation timescales. I also assess our current understanding of the (initial) binary fraction in star clusters and the shape of the stellar initial mass function at the low-mass end in the low-metallicity environment of the Large Magellanic Cloud. Finally, I question the validity of our assumptions leading to dynamical cluster mass estimates. I conclude that it seems imperative that observers, modellers and theorists combine efforts and exchange ideas and data freely for the field to make a major leap forward.

scholarly journals Size diversity of old Large Magellanic Cloud clusters as determined by internal dynamical evolution

2019 ◽  
Vol 3 (12) ◽  
pp. 1149-1155 ◽  
Author(s):  
F. R. Ferraro ◽  
B. Lanzoni ◽  
E. Dalessandro ◽  
M. Cadelano ◽  
S. Raso ◽  
...  
Keyword(s):  
Dynamical Evolution ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Clusters ◽  
Size Diversity
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