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Mass Segregation in the Young SMC Cluster NGC 330

Published online by Cambridge University Press:  03 August 2017

Marco Sirianni ,
Antonella Nota ,
Guido De Marchi ,
Claus Leitherer  and
Mark Clampin
Marco Sirianni
Affiliation:
Johns Hopkins University, 3400 N Charles St, Baltimore MD 21218, USA
Antonella Nota
Affiliation:
STScI/ESA, 3700 San Martin Drive, Baltimore MD 21218, USA
Guido De Marchi
Affiliation:
STScI/ESA, 3700 San Martin Drive, Baltimore MD 21218, USA
Claus Leitherer
Affiliation:
STScI, 3700 San Martin Drive, Baltimore MD 21218, USA
Mark Clampin
Affiliation:
STScI, 3700 San Martin Drive, Baltimore MD 21218, USA

Abstract

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We present a new study of the low end of the stellar IMF of NGC 330, the richest young star cluster in the Small Magellanic Cloud (SMC). Using deep broadband images taken with the HST/WFPC2 we have derived the cluster's luminosity function and constructed the initial mass function (IMF) in the mass range 1 − 7M⊙. We have investigated the IMF as a function of the radial distance from the cluster center. We find that, after correction for background contamination, the IMF is fairly homogeneous with a slope slightly steeper than Salpeter's in the central regions of the cluster (< 40″) but becomes increasingly steeper with distance, indicating a preponderance of massive stars in the core of the cluster. NGC 330 is one of the first clusters for which evidence of mass segregation is directly found.

Type
Part 4. Star Cluster Formation and Evolution: Theory and Observation
Information
Symposium - International Astronomical Union , Volume 207: Extragalactic Star Clusters , 2002 , pp. 687 - 690
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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