Cool Gas in Clusters of Galaxies
| dc.creator | Donahue, Megan | |
| dc.creator | Voit, G. Mark | |
| dc.date | 2003-07-31 | |
| dc.date.accessioned | 2026-07-07T02:09:07Z | |
| dc.date.available | 2026-07-07T02:09:07Z | |
| dc.description | Early X-ray observations suggested that the intracluster medium cools and condenses at the centers of clusters, leading to a cooling flow of plasma in the cluster core. The increased incidence of emission-line nebulosity, excess blue light, AGN activity, and molecular gas in the cores of clusters with short central cooling times seemed to support this idea. However, high-resolution spectroscopic observations from XMM-Newton and Chandra have conclusively ruled out simple, steady cooling flow models. We review the history of this subject, the current status of X-ray observations, and some recent models that have been proposed to explain why the core gas does not simply cool and condense. | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0308006 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0308006 | |
| dc.identifier | 2003 Carnegie Observatory Astrophysics Series, Vol 3: Clusters of Galaxies: Probes of Cosmological Structure and Galaxy Evolution, eds. J. S. Mulchaey, A. Dressler and A. Oemler (Cambridge: Cambridge University Press) | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/6316 | |
| dc.subject | Astrophysics | |
| dc.title | Cool Gas in Clusters of Galaxies | |
| dc.type | text |