The Physical Origin of Galaxy Scaling Relations
| dc.creator | White, Simon D. M. | |
| dc.date | 1997-02-25 | |
| dc.date.accessioned | 2026-07-07T02:22:59Z | |
| dc.date.available | 2026-07-07T02:22:59Z | |
| dc.description | A standard paradigm is now available for the recent evolution (z < 10) of structure on galactic and larger scales. Most of the matter is assumed to be dark and dissipationless and to cluster hierarchically from gaussian initial conditions. Gas moves under the gravitational influence of this dark matter, settling dissipatively at the centres of dark halos to form galaxies. The evolution of the dark matter component has been studied extensively by N-body simulations. The abundances, density profiles, shape and angular momentum distributions and the formation histories of the dark halo population can all be predicted reliably for any hierarchical cosmogony. The systematic variation of these properties with halo mass can produce scaling relations in the galaxy population. Simple hypotheses for how galaxies condense within dark halos lead to characteristic luminosities, sizes, and spins which are close to those of real spiral and elliptical galaxies. Furthermore, correlations similar to the Tully-Fisher, Faber-Jackson and luminosity-metallicity relations arise quite naturally. A quantitative explanation of the fundamental plane of elliptical galaxies appears within reach. | |
| dc.description | 12 pages. Invited review for the 3rd ESO-VLT Workshop "Galaxy Scaling Relations: Origins, Evolution and Applications", Garching, 18-20 November 1996 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9702214 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9702214 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/11080 | |
| dc.subject | Astrophysics | |
| dc.title | The Physical Origin of Galaxy Scaling Relations | |
| dc.type | text |