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Central Densities of Star Clusters in the Magellanic Clouds

Comparison With Our Galaxy

Published online by Cambridge University Press:  25 May 2016

M. Kontizas ,
D. Gouliermis  and
E. Kontizas
M. Kontizas
Affiliation:
Section of Astrophysics, Astronomy & Mechanics, Department of Physics, University of Athens, Panepistimiopolis GR-157 83, Athens, Greece
D. Gouliermis
Affiliation:
Astronomical Institute, National Observatory of Athens, P.O.BOX 20048, 118 10 Athens, Greece
E. Kontizas
Affiliation:
Astronomical Institute, National Observatory of Athens, P.O.BOX 20048, 118 10 Athens, Greece

Abstract

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The way star cluster systems in galaxies are forming and survive seem to depend on the relation of the central density ρ (at half mass radius) of each cluster with its galactocentric distance Rgc. It is found that this relation takes the form of: The cluster systems of our Galaxy and of the two Magellanic Clouds, have been investigated. We have taken the cluster system of the conventional globulars of our Galaxy whereas the young and old systems of clusters in the LMC and SMC were treated separately. The radial distributions of central densities and half mass radii were found for all these systems showing a definite trend which depends on: (α) The total mass of the parent galaxy & (β) The age of the cluster system (young - old). It therefore appears that the total mass and/or the morphology of the parent galaxy plays a major role on the loci where clusters survive and form.

Type
Posters: Observations of Star Clusters
Information
Symposium - International Astronomical Union , Volume 174: Dynamical Evolution of Stars Clusters , 1996 , pp. 335 - 336
Copyright
Copyright © Kluwer 1996 

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