The Effects of Cluster Environment on the Chemical Evolution of Galaxies

1999 ◽  
pp. 203-203
Author(s):  
L. S. Pilyugin ◽  
F. Ferrini
Keyword(s):  
Chemical Evolution ◽  
Evolution Of Galaxies ◽  
Cluster Environment

scholarly journals The effects of cluster environment on the chemical evolution of galaxies - II. NGC 4254

1994 ◽  
Vol 266 (2) ◽  
pp. 421-430 ◽  
Author(s):  
R. B. C. Henry ◽  
B. E. J. Pagel ◽  
G. L. Chincarini
Keyword(s):  
Chemical Evolution ◽  
Evolution Of Galaxies ◽  
Cluster Environment

scholarly journals The effects of cluster environment on the chemical evolution of galaxies -- III. NGC 753

1996 ◽  
Vol 283 (2) ◽  
pp. 635-647 ◽  
Author(s):  
R. B. C. Henry ◽  
C. Balkowski ◽  
V. Cayatte ◽  
M. G. Edmunds ◽  
B. E. J. Pagel
Keyword(s):  
Chemical Evolution ◽  
Evolution Of Galaxies ◽  
Cluster Environment

scholarly journals The effects of cluster environment on the chemical evolution of galaxies - I. NGC 4303

1992 ◽  
Vol 258 (2) ◽  
pp. 321-333 ◽  
Author(s):  
R. B. C. Henry ◽  
B. E. J. Pagel ◽  
D. F. Lasseter ◽  
G. L. Chincarini
Keyword(s):  
Chemical Evolution ◽  
Evolution Of Galaxies ◽  
Cluster Environment

scholarly journals Measuring the Evolution of the M/L ratio from the Fundamental Plane in Cl 0024+16 at z=0.39

1996 ◽  
Vol 171 ◽  
pp. 233-240 ◽  
Author(s):  
Marijn Franx ◽  
Pieter G. van Dokkum
Keyword(s):  
Luminosity Function ◽  
Evolutionary Models ◽  
Early Type ◽  
Rich Cluster ◽  
Fundamental Plane ◽  
Evolution Of Galaxies ◽  
Cluster Environment ◽  
Dynamical Properties ◽  
The Rich

The existence of the Fundamental Plane of early-type galaxies implies that the M/L ratios of early-types are well behaved. It provides therefore an important tool to measure the evolution of the M/L ratio with redshift. These measurements, in combination with measurements of the evolution of the luminosity function, can be used to constrain the mass evolution of galaxies.We present the Fundamental Plane relation measured for galaxies in the rich cluster CL 0024+16 at z=0.391. The galaxies satisfy a tight Fundamental Plane, with relatively low scatter (15 %). The M/L is 31 ± 12 % lower than the M/L measured in Coma, which is consistent with simple evolutionary models. Hence, galaxies with very similar dynamical properties existed at a z=0.4.More, and deeper data are needed to measure the evolution of the slope and the scatter of the Fundamental Plane to higher accuracy. Furthermore, data on the richest nearby clusters would be valuable to test the hypothesis that the Fundamental Plane is independent of cluster environment.

scholarly journals ASCA Observations of the Abell 496 Cluster of Galaxies

1998 ◽  
Vol 188 ◽  
pp. 304-305
Author(s):  
I. Hatsukade ◽  
J. Ishizaka ◽  
M. Yamauchi ◽  
K. Takagishi
Keyword(s):  
Mass Flow Rate ◽  
Chemical Evolution ◽  
Mass Flow ◽  
Relative Abundance ◽  
Flow Rate ◽  
Metal Distribution ◽  
Rich Cluster ◽  
Cooling Flow ◽  
Evolution Of Galaxies ◽  
Cluster Of Galaxies

The metal in the intracluster medium (ICM) has been ejected or stripped from galaxies. Thus measurements of the metal distribution and the relative abundance of elements, in particular Si/Fe, are important to study the evolution of galaxies, as well as to study the chemical evolution of the ICM. We present the results from ASCA observations of Abell 496 cluster of galaxies. A496 is a nearby rich cluster with a central cD galaxy. At the redshift z=0.0327 of A496, 1 arcmin is 53kpc, where we assumed H0 = 50kms−1Mpc−1, q0 = 0.5. A496 is known as a cooling flow cluster. Edge and Stewart (1991) obtained the mass flow rate of and the cooling radius of 177 ± 52kpc.

scholarly journals Relations between the galactic evolution and the stellar evolution

1984 ◽  
Vol 105 ◽  
pp. 541-548 ◽  
Author(s):  
Jean Audouze
Keyword(s):  
Chemical Evolution ◽  
Stellar Evolution ◽  
Galactic Evolution ◽  
Evolution Of Galaxies ◽  
The Impact

The question which has been raised in many chapters of this book is about the existence of constraints on stellar evolution coming from related topics like cosmology or in the case of the present chapter the chemical evolution of the galaxies. As it will be seen in this contribution it seems wiser to consider that chemical evolution of galaxies is indeed related to the problem of stellar evolution discussed here but is not going to provide as many constraints on it as one would expect. The purpose of this presentation is therefore to outline the principal relations between these two fields and to discuss the impact of some recent works on them.

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