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Planetary Nebulae in Extragalactic Young Star Clusters

Published online by Cambridge University Press:  01 December 2006

S. S. Larsen  and
T Richtler
S. S. Larsen
Affiliation:
Astronomical Institute, University of Utrecht, Princetonplein 5, 3584 CC, Utrecht, The Netherlands, email: larsen@astro.uu.nl
T Richtler
Affiliation:
Astronomy Group, Universidad de Concepción, Departamento de Física, Casilla 160-C, Concepción, Chile, email: tom@mobydick.cfm.udec.cl
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Abstract

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We have recently obtained optical spectra for a large sample of young and intermediate-age star clusters in several nearby galaxies. The main aim of this programme is to carry out a detailed test of photometric and spectroscopic age- and metallicity indicators, but a first inspection of the data has also revealed emission lines in 3 clusters with ages of 30 Myrs or older. We identify these three objects as likely Planetary Nebula (PN) candidates and discuss their properties. Based on the cluster ages, the progenitor stars had initial masses in the range 3 to 7 M⊙, while the PN central stal luminosities and temperatures (estimated from emission line fluxes) are consistent with current masses close to 0.60 M⊙. These objects represent a rare opportunity to study PNe whose progenitor stars are known to be of intermediate masses, although detailed analysis is challenging because of the strong underlying stellar continuum from the cluster stars. Detection of 3 PNe in our sample appears consistent with expectations from stellar evolutionary theory.

Keywords

stars: AGB and post-AGBgalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 453 - 454
Copyright
Copyright © International Astronomical Union 2007

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