New Aspects of Young Magellanic Cloud Clusters

Integral fluxes (Bolometric and U, B, V) are computed in a completely theoretical frame in order to investigate the structural properties and stellar content of coeval stellar systems of various ages and metal abundance. Some results concerning the problem of the color gap in the distribution of the sample of Magellanic Cloud clusters are discussed.

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Blue–violet spectral evolution of young Magellanic Cloud clusters

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/276.4.1155 ◽

1995 ◽

Cited By ~ 3

Keyword(s):

Magellanic Cloud ◽

Spectral Evolution ◽

Cloud Clusters

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Star clusters in the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900200259 ◽

1991 ◽

Vol 148 ◽

pp. 161-164 ◽

Cited By ~ 1

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.

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The Abundance of the LMC Globular Cluster NGC 2213

Symposium - International Astronomical Union ◽

10.1017/s0074180900043163 ◽

1988 ◽

Vol 126 ◽

pp. 579-580

Author(s):

Doug Geisler

Keyword(s):

Globular Cluster ◽

Main Sequence ◽

High Accuracy ◽

Magellanic Cloud ◽

New Technique ◽

Distance Modulus ◽

Ccd Photometry ◽

Cloud Clusters ◽

A New Technique ◽

Using Data

A new technique for determining accurate abundances in distant giants - Washington CCD photometry - has been applied to the intermediate-age LMC globular cluster NGC 2213. An abundance of −0.40 ± 0.15 was found from the analysis of 42 giants with V < 20, using data obtained with the 1.5 m telescope. Combined with published main-sequence photometry, the derived abundance indicates a true LMC distance modulus of 18.2 ± 0.2. A likely CN strong giant near the tip of the giant branch is identified. Abundances are also derived for a sample of 27 field giants. Results indicate that one could determine both the age and abundance of Magellanic Cloud clusters with high accuracy from Washington photometry using the 4 m in less than one hour of observing time per cluster.

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