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Galaxy Harassment—Interactions for the 90s

Published online by Cambridge University Press:  25 May 2016

George Lake and
Ben Moore
George Lake
Affiliation:
Department of Astronomy, University of Washington, Box 351580, Seattle WA 98195, USA
Ben Moore
Affiliation:
Department of Physics, University of Durham, Durham City, DH1 3LE, UK

Extract

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The origin of the Hubble sequence remains a long-standing puzzle in astronomy. Giant galaxies range from slowly-rotating dense ellipticals to thin late-type spiral disks. At the faint end, there are two distinct classes of “ellipticals/spheroids” that are easily separated in plots of nearly any two of their properties, such as central surface brightness versus luminosity (Ferguson and Binggeli 1994; Kormendy 1985). The elliptical class includes the bright giants and extends to the rare high surface brightness “dwarf ellipticals”, M32 being the prototype. The “spheroidal” galaxies have low surface brightnesses and are all ≳3 magnitudes fainter than L ∗, the characteristic break in the luminosity function. The dwarf spheroidal galaxies (dSph) in our Local Group of galaxies with magnitudes in the range −8≳M B≳ - 12 are often considered to be the low luminosity extreme of this sequence, but nearly all other known galaxies in this class reside in clusters.

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