Influence of Cooling Flows and Galactic Motion on the Iron Distribution in Clusters of Galaxies

1995 ◽  
Vol 452 ◽  
pp. 177 ◽  
Author(s):  
Yutaka Fujita ◽  
Hideo Kodama
Keyword(s):  
Clusters Of Galaxies ◽  
Iron Distribution ◽  
Cooling Flows

scholarly journals A ROSAT study of the cores of clusters of galaxies -- I. Cooling flows in an X-ray flux-limited sample

1998 ◽  
Vol 298 (2) ◽  
pp. 416-432 ◽  
Author(s):  
C. B. Peres ◽  
A. C. Fabian ◽  
A. C. Edge ◽  
S. W. Allen ◽  
R. M. Johnstone ◽  
...  
Keyword(s):  
Clusters Of Galaxies ◽  
Limited Sample ◽  
X Ray ◽  
Cooling Flows

scholarly journals Cooling flows in clusters of galaxies

1991 ◽  
Vol 2 (3-4) ◽  
pp. 191-226 ◽  
Author(s):  
A. C. Fabian ◽  
P. E. J. Nulsen ◽  
C. R. Canizares
Keyword(s):  
Clusters Of Galaxies ◽  
Cooling Flows

scholarly journals Color Maps of A 1795 and A 2597 - Cooling Flow Cluster Central Galaxies with Active Nuclei

1989 ◽  
Vol 134 ◽  
pp. 460-461
Author(s):  
W. Romanishin
Keyword(s):  
Star Formation ◽  
Clusters Of Galaxies ◽  
Nuclear Activity ◽  
X Ray ◽  
Cluster Galaxies ◽  
Cooling Flows ◽  
Cooling Flow ◽  
Show Evidence ◽  
The Subject ◽  
Optical Manifestation

The subject of cooling flows in clusters of galaxies remains a controversial one, primarily because many clusters which have large x-ray derived mass inflow rates do not show any optical manifestation of the inflow or of the final fate of the gas. However, a handful of cooling flow clusters do show extended blue continuum regions indicative of current star formation which may be caused by the cooling flows (Romanishin 1987, Romanishin and Hintzen 1988), while another group show spectral evidence of star formation (O'Connell and McNamara 1988). Most of the cluster galaxies which show evidence of star formation also show nuclear activity, in the form of radio emission.

scholarly journals X-Rays from Galaxies and Clusters of Galaxies: Observations and Phenomenology

1987 ◽  
Vol 117 ◽  
pp. 165-181 ◽  
Author(s):  
C. R. Canizares
Keyword(s):  
Direct Evidence ◽  
Temperature Profiles ◽  
Clusters Of Galaxies ◽  
X Rays ◽  
Early Type ◽  
X Ray ◽  
Cluster Galaxies ◽  
Cooling Flows ◽  
Hot Gas ◽  
Relevant Work

X-Ray observations of galaxies and clusters can, in principle, trace the binding mass in these systems. I review some of the relevant work. The mass of hot gas in rich clusters is comparable to or exceeds the mass in visible stars. This proportion of gas to stellar material could be universal, although there is no direct evidence that it must be. Studies of the distribution of the gas indicate the presence of dark matter in the envelopes of some dominant cluster galaxies, most notably M87. The M/LB values increase with radius to values of ∼ 400–600 M⊙/L⊙. Uncertainties in the temperature distribution of the gas have hampered these analyses and have made it difficult to draw definitive conclusions about the binding mass in clusters. Recent work on Coma suggests that M/L is falling with radius and the total M/L for the cluster may be as low as ∼ 120. Studies of early type galaxies show that many contain hot gas with temperatures ∼107 K. There is evidence for the existence of cooling flows, and gravity rather than supernovae may be the dominant source of energy that heats the gas. The deduced binding masses for several bright galaxies are uncertain because of the unknown temperature profiles. Values of M/LB ≃ 20–30 within ∼ 30–40 kpc are indicated if one assumes isothermality, but values as low as 5 and as high as 100 are allowed. With better models one may be able to reduce these uncertainties.

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