Abstract
The observable properties of star clusters hold vital information concerning the star formation process. In this introductory chapter we review the properties of open clusters within the Galaxy. Starting with the most basic properties of open clusters, such as age, mass and metallicity, we then move onto a discussion of how these properties vary depending on the number density, cluster mass and spatial distribution across the Galaxy. In addition to these observables, we also describe methods of selecting members of open clusters through the use of proper motion and radial velocity kinematic information, and demonstrate their usage in highlighting dynamical evolutionary processes, for example, mass segregation. Finally, we end this chapter with a discussion of unbound stellar populations, namely OB associations, and their relation to molecular clouds within the Galaxy.
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Notes
- 1.
Estimating stellar ages (and thus the clusters in which they reside) is a complex topic and the reader is referred to Soderblom (2010) for a comprehensive review.
- 2.
Ivan King once cautioned to be very careful with compilations. They are extremely valuable, but they are inherently heterogeneous in terms of both the content and the quality of the entries.
- 3.
All of the clusters in Fig. 8.4 are in motion about the Milky Way. Those clusters seen far from the disc mid-plane are on orbits with larger average z-components than most of those seen in the disc. Nonetheless, they also pass through and interact with the disc, just on a less frequent basis.
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Mathieu, R.D. (2015). Introduction to Open Clusters. In: Meyer, M., Eyer, L., Bell, C. (eds) Dynamics of Young Star Clusters and Associations. Saas-Fee Advanced Course, vol 42. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-47290-3_8
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