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Stellar Populations in the Magellanic Clouds

Published online by Cambridge University Press:  07 August 2017

M.W. Feast
M.W. Feast*
Affiliation:
Department of Astronomy, University of Cape Town, Private Bag, Rondebosch 7700, South Africa (mwf@uctvax.uct.ac.za)

Abstract

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There seems to be no strong evidence that the young globular clusters in the MC have metallicities differing significantly from the metallicities of MC field stars of the same age. The old globular clusters in the LMC are of the same age as, or slightly younger than, those in the outer halo of our Galaxy. It is suggested that the increase in the SFR in the LMC ~ 4 Gyr ago was related to the collapse of the system to a plane. Evidence for a spread in metallicities amongst young stars in either Cloud remains tentative. There is no strong evidence for bursts of star formation being triggered by LMC-SMC-Galaxy interactions but the possibility is raised that the SFR in the SMC has been strongly affected by this interaction.

Type
Session 4: Stellar Populations in Local Group Galaxies
Information
Symposium - International Astronomical Union , Volume 164: Stellar Populations , 1995 , pp. 153 - 163
Copyright
Copyright © Kluwer 1995 

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