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Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/207815
- Elliptical and disc galaxy structure, and modern scaling laws
- Graham, Alister W.
- A century ago, in 1911 and 1913, Plummer and then Reynolds introduced their models to describe the radial distribution of stars in 'nebulae'. This article reviews the progress since then, providing both an historical perspective and a contemporary review of the stellar structure of bulges, discs and elliptical galaxies. The quantification of galaxy nuclei, such as central mass deficits and excess nuclear light, plus the structure of dark matter halos and cD galaxy envelopes, are discussed. Issues pertaining to spiral galaxies including dust, bulge-to-disc ratios, bulgeless galaxies, bars and the identification of pseudobulges are also reviewed. An array of modern scaling relations involving sizes, luminosities, surface brightnesses and stellar concentrations are presented, many of which are shown to be curved. These 'redshift zero' relations not only quantify the behavior and nature of galaxies in the Universe today, but are the modern benchmark for evolutionary studies of galaxies, whether based on observations, N-body-simulations or semi-analytical modelling. For example, it is shown that some of the recently discovered compact elliptical galaxies at 1.5 < z < 2.5 may be the bulges of modern disc galaxies.
- Publication type
- Book chapter
- Research centre
- Swinburne University of Technology. Faculty of Information and Communication Technologies. Centre for Astrophysics and Supercomputing
- Planets, stars and stellar systems / T. D. Oswalt, I. S. McLean, H. E. Bond, L. French, P. Kalas, M. Barstow, G. F. Gilmore and W. Keel (eds.), Chapter 2, pp. 91-139
- Publication year
- cD galaxies; Compact galaxies; Dark matter haloes; Elliptical galaxies; Galaxy scaling relations; Galaxy structure; Pseudobulges; Spiral galaxies
- Publisher URL
- Copyright © Springer Science+Business Media Dordrecht 2013.
- Research Projects
Massive black holes in dense star clusters, Australian Research Council grant number DP110103509
- Peer reviewed