Abstract
Hidden in the bewildering details of galaxy morphology are clues to how galaxies formed and have evolved over a Hubble time. This article reviews the phenomenology of galaxy morphology and classification using an extensive set of illustrations to delineate as many types as possible and to show how different types connect to various physical processes and characteristics. The old classification systems are refined, and new types introduced, as the explosion in available morphological data has modified our views on the structure and evolution of galaxies.
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Notes
- 1.
- 2.
Van den Bergh (2009a) shows that E0–E4 galaxies are more luminous on average than are E5–E7 galaxies, suggesting that all E7 galaxies (and not many have been recognized) are actually S0 galaxies. Van den Bergh argues that genuine E galaxies may be no more flattened than E6.
- 3.
After this chapter was completed, Kormendy and :̧def mbox :̧def :̱mbox mbox Bender:̱mbox (2012) suggested that NGC 4638 represents a harassed disk galaxy in a dense part of the Virgo Cluster and is not an E galaxy with an acquired or imbedded disk.
- 4.
In a study of galactic nuclei, van den Bergh (1995) proposed the notation “NB” for nuclear bars, although what he refers to are not the same as the features described here. However, the presence or absence of a nucleus is an important morphological issue that may be connected to evolutionary history, as noted by van den Bergh.
- 5.
In contrast to van den Bergh’s study of RSA S0 galaxies, Laurikainen et al. (2010) found that the absolute K s -band magnitudes of a well-defined sample of S0s are similar to those of early-type spirals in the OSUBSGS sample. The sample was mostly drawn from RC3 and includes some galaxies classified as ellipticals in RC3 and as S0s in the RSA (see Sect. 12).
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Buta, R.J. (2013). Galaxy Morphology. In: Oswalt, T.D., Keel, W.C. (eds) Planets, Stars and Stellar Systems. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-5609-0_1
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