Titlebook: Galaxy Evolution in Groups and Clusters; A JENAM 2002 Worksho Catarina Lobo,Margarida Serote Roos,Andrea Biviano Book 2003 Springer Science

Morose

The Evolutionary Status of Early-Type Galaxies in Abell 2390ubsample of 14 galaxies with morphological and structural parameters from HST, we also investigate the evolution of the Kormendy relation and the Fundamental Plane. We find a mild luminosity evolution of the early-type galaxies in Abell 2390: our objects are on average brighter by .. ∼ 0.4 mag.

Palpitation

etidronate

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The Orbits of Cluster Galaxy Populations as Evolutionary Constraints(ENACS). We use ellipticals and S0s as tracers of the cluster potential, and solve the Jeans equation assuming isotropic orbits. Such an assumption is justified by the analysis of the shape of the velocity distribution of ellipticals and S0s. We find that the cluster mass profile is consistent with

majestic

Morphology and Luminosity Segregations in Galaxy Groupsthe Nearby Optical Galaxy sample, by means of hierarchical and percolation ‘friends-of-friends’ methods. We find that earlier-type (brighter) galaxies are more clustered and lie closer to the group centers, both in position and in velocity, than later-type (fainter) galaxies. Spatial segregations ar

Scleroderma

The Velocity Dispersion In The X-Ray Scaling Lawsand the optical velocity dispersion σ. We obtained redshifts for the fainter members of these groups. We find that X-ray bright groups have more members and higher velocity dispersions on average. Using the fainter group members and Monte Carlo tests, we define the number of group members required t

带来

The Evolution of Brightest Cluster Galaxieseir use as cosmological probes. BCGs form a unique galaxy population. They are located near the gravitational centre of galaxy clusters and are the most massive galaxies in the universe, being some 10 times more luminous than L. systems. Historically, BCGs have been credited with small intrinsic dis

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继而发生

Structural Properties of Brightest Cluster Galaxiesface brightness profiles of BCGs out to large radii is critical for understanding the processes driving their formation. The form of the profiles yields information about the current dynamical state, constrains the accretion history of these galaxies, and places limits on any radially symmetric comp