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Stellar Populations in the Nuclei of Spiral Galaxies

Published online by Cambridge University Press:  30 March 2016

R. W. O’Connell
R. W. O’Connell*
Affiliation:
Astronomy Department, University of Virginia, Charlottesville, Virginia USA

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Spiral galaxies are a composite of two dynamical population types: the spheroidal and disk populations. These can be studied in isolation in E and Irr galaxies, respectively. It is natural to expect that the combination in a spiral of a dense spheroidal population, having a deep central potential well, with a repository of interstellar gas and dust in the disk gives rise to special conditions not usually found in E or Irr galaxies. And in fact, we find spectacular concentrations of star forming regions in some spiral nuclei.

In this review, I will limit most of the discussion to later spiral types which are classified as “intermediate” in the Yerkes system (Morgan and Osterbrock 1969). Types earlier than Sbc usually have “k-nuclei,” where the spheroidal population dominates; excellent reviews are available for these types (van den Bergh 1975, Faber 1977).

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 6 , 1983 , pp. 147 - 156
Copyright
Copyright © Reidel 1983

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