BVRI photometry of star clusters in the BOK region of the Large Magellanic Cloud

1987 ◽  
Vol 94 ◽  
pp. 372 ◽  
Author(s):  
Gonzalo Alcaino ◽  
William Liller
Keyword(s):  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Catalogue of Large Magellanic Cloud star clusters observed in the Washington photometric system

2016 ◽  
Vol 586 ◽  
pp. A41 ◽  
Author(s):  
T. Palma ◽  
L. V. Gramajo ◽  
J. J. Clariá ◽  
M. Lares ◽  
D. Geisler ◽  
...  
Keyword(s):  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Photometric System

scholarly journals The VISCACHA survey – II. Structure of star clusters in the Magellanic Clouds periphery

2020 ◽  
Vol 498 (1) ◽  
pp. 205-222
Author(s):  
João F C Santos ◽  
Francisco F S Maia ◽  
Bruno Dias ◽  
Leandro de O Kerber ◽  
Andrés E Piatti ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Structural Parameters ◽  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
The Core ◽  
Optical Images ◽  
Low Surface Brightness ◽  
Homogeneous Set ◽  
Stellar Density

ABSTRACT We provide a homogeneous set of structural parameters of 83 star clusters located at the periphery of the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC). The clusters’ stellar density and surface brightness profiles were built from deep, AO assisted optical images, and uniform analysis techniques. The structural parameters were obtained from King and Elson et al. model fittings. Integrated magnitudes and masses (for a subsample) are also provided. The sample contains mostly low surface brightness clusters with distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and SMC centres, respectively. We analysed their spatial distribution and structural properties, comparing them with those of inner clusters. Half-light and Jacobi radii were estimated, allowing an evaluation of the Roche volume tidal filling. We found that: (i) for our sample of LMC clusters, the tidal radii are, on average, larger than those of inner clusters from previous studies; (ii) the core radii dispersion tends to be greater for LMC clusters located towards the southwest, with position angles of ∼200° and about ∼5° from the LMC centre, i.e. those LMC clusters nearer to the SMC; (iii) the core radius evolution for clusters with known age is similar to that of inner clusters; (iv) SMC clusters with galactocentric distances closer than 4 kpc are overfilling; (v) the recent Clouds collision did not leave marks on the LMC clusters’ structure that our analysis could reveal.

scholarly journals Properties of two star clusters of the LMC: NGC 2164, NGC 1850

1991 ◽  
Vol 148 ◽  
pp. 219-221
Author(s):  
A. Vallenari ◽  
C. Chiosi ◽  
G. Bertelli ◽  
G. Meylan ◽  
S. Ortolani
Keyword(s):  
Star Clusters ◽  
Theoretical Models ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Luminosity Functions ◽  
Stellar Models ◽  
Convective Overshoot

We present the photometry of two clusters NGC 2164 and NGC 1850 located in the Large Magellanic Cloud (LMC). The ages are determined taking into account the presence either of convective overshoot or of semiconvection in the stellar models. The experimental luminosity functions are compared with the theoretical models.

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.

Ages of star clusters in a section of the Large Magellanic Cloud

1974 ◽  
Vol 79 ◽  
pp. 1365 ◽  
Author(s):  
S. Baird ◽  
P. Flower ◽  
P. Hodge ◽  
P. Szkody
Keyword(s):  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

457 New Star Clusters of hte Large Magellanic Cloud

1966 ◽  
Vol 71 ◽  
pp. 363 ◽  
Author(s):  
P. W. Hodge ◽  
J. A. Sexton
Keyword(s):  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals A BVRI Photometric Study of Star Clusters in the Bok Region of the LMC

1984 ◽  
Vol 108 ◽  
pp. 49-50
Author(s):  
Gonzalo Alcaino ◽  
William Liller
Keyword(s):  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Photometric Study ◽  
Excellent Opportunity ◽  
Total Luminosity ◽  
Wide Range

The large number of star clusters in the Large Magellanic Cloud provides us with an excellent opportunity to understand well this neighboring galaxy. The large variety of integrated cluster colors present suggests a wide range in evolutionary stages, and several studies have established vague relationships between their location in the LMC and properties including color, total luminosity and metallicity.

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