Abstract
Stellar populations encode the star-formation history and chemical evolution of a system. This chapter reviews the development of the concept of stellar populations and the current understanding of the resolved stellar populations in the Local Group, with an emphasis on the older stars and serves to introduce the topics of several later chapters.
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Notes
- 1.
Most usefully, the (U − B) color excess, normalized to a star with (B − V) = 0.6 on the main sequence of the Hyades cluster (Sandage and Eggen 1959)
- 2.
More recently, this component has been identified with the bulge of M31 and also with accreted material from a satellite of M31; see Sect. 3.2.2 below.
- 3.
The primary motivation was to understand how the evolution of the stellar content of galaxies affected the use of galaxy counts to infer cosmological parameters.
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Acknowledgements
I acknowledge support through grants AST-0908326 and CDI-1124403 from the National Science Foundation. I thank the Aspen Center for Physics, supported by NSF Grant 1066293, for hospitality while I completed this chapter.
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Wyse, R.F.G. (2013). Stellar Populations. In: Oswalt, T.D., Gilmore, G. (eds) Planets, Stars and Stellar Systems. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-5612-0_1
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