Detection of the helium flash gap in the integrated (U - B) versus (B - V) diagram for 624 Large Magellanic Cloud clusters

1991 ◽  
Vol 381 ◽  
pp. L51 ◽  
Author(s):  
E. Bica ◽  
H. Dottori ◽  
J. F. C., Jr. Santos ◽  
J. J. Claria ◽  
A. Piatti
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud 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 Blue Straggler Stars Beyond the Milky Way. III. Detection of Evolved Blue Straggler Candidates in Large Magellanic Cloud Clusters

2018 ◽  
Vol 156 (3) ◽  
pp. 110 ◽  
Author(s):  
Chengyuan Li ◽  
Licai Deng ◽  
Kenji Bekki ◽  
Jongsuk Hong ◽  
Richard de Grijs ◽  
...  
Keyword(s):  
Milky Way ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Clusters ◽  
Blue Straggler

Testing Intermediate-Age Stellar Evolution Models with VLT Photometry of Large Magellanic Cloud Clusters. II. Analysis with the Yale Models

2003 ◽  
Vol 125 (2) ◽  
pp. 754-769 ◽  
Author(s):  
Jong-Hak Woo ◽  
Carme Gallart ◽  
Pierre Demarque ◽  
Sukyoung Yi ◽  
Manuela Zoccali
Keyword(s):  
Stellar Evolution ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Clusters

scholarly journals First Estimates of the Fundamental Parameters of Three Large Magellanic Cloud Clusters

2011 ◽  
Vol 123 (903) ◽  
pp. 519-530 ◽  
Author(s):  
Andrés E. Piatti ◽  
Juan J. Clariá ◽  
María Celeste Parisi ◽  
Andrea V. Ahumada
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Fundamental Parameters ◽  
Cloud Clusters

Mass to Light Ratios of Large Magellanic Cloud Clusters

1991 ◽  
pp. 191-192 ◽  
Author(s):  
Mario Mateo ◽  
Douglas Welch ◽  
Phil Fischer
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cloud Clusters

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.

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