Scientists involved in the GIF project combined the large high-resolution N-body simulations with semi-analytical models to study formation and evolution of galaxies. This picture, created by Joerg Colberg and Antonaldo Diaferio, shows the population of galaxies superposed on dark-matter distribution (grey-colored) in a small region of 21x21x8 (Mpc/h)³. (See also the picture of dark-matter distribution below.) Galaxies are shown as circles colour-coded according to their star formation rate: the sequence red, yellow, green and blue represents an increasing rate of star formation. At early times (top left panel) there exist only a few galaxies forming stars at a very high rate. As time goes on, from z=3 to z=0, more galaxies form and, at the same time, some galaxies run out of gas, form fewer stars and become green, yellow and red. At the present time (z=0), red galaxies populate the central region of the cluster, whereas blue galaxies can be found in the outskirts of the system. This is very similar to what is observed in the real Universe.

• The Large-scale Distribution of Galaxies, G. Kauffmann,A. Diaferio, Annual Report of the MPA, 1998, pp.25-29
  
  
• Clustering of Galaxies in a Hierarchical Universe: I. Methods and Results at z=0, G. Kauffmann, J.M. Colberg, A. Diaferio, S.D.M. White, 1999, MNRAS, 303, 188-206,
  Preprint astro-ph/9805283
  
  
• Clustering of Galaxies in a Hierarchical Universe: II. Evolution to High Redshift, G. Kauffmann, J.M. Colberg, A. Diaferio, S.D.M. White, 1999, MNRAS, 307, 529-536,
  Preprint astro-ph/9809168
  
  
• Clustering of Galaxies in a Hierarchical Universe: III. Mock Redshift Surveys, A. Diaferio, G. Kauffmann, J.M. Colberg, S.D.M. White, 1999, MNRAS, 307, 537-552,
  Preprint astro-ph/9812009
  
  
• The Spatial and Kinematic Distributions of Cluster Galaxies in a LCDM Universe - Comparison with Observations, A. Diaferio, G. Kauffmann, M. L. Balogh, S.D.M. White, D. Schade and E. Ellingson MNRAS, in press,
  Preprint astro-ph/0005485
  
  
• Ab Initio Formation of Galaxies, Groups and Large-Scale Structure, A. Diaferio, Invited talk at the IAU Colloquium 174 "Small Galaxy Groups", Turku, Finland, 13-18 June 1999, M. Valtonen and C. Flynn editors, astro-ph/9908263
  
  
• Mass estimation in the outer regions of galaxy clusters, A. Diaferio, 1999, MNRAS, 309, 610-622, astro-ph/9906331
  
  
• Topology and Geometry of the CfA2 Redshift survey, J. Schmalzing, A. Diaferio, 2000, MNRAS, 312, 638-648, astro-ph/9910228
  
  
• Analytic model for galaxy and dark matter clustering, U. Seljak, 2000, MNRAS, 318, 203-213, astro-ph/0001493
  
  
• Non-linear Stochastic Galaxy Biasing in Cosmological Simulations, R. S. Somerville, G. Lemson, Y. Sigad, A. Dekel, G. Kauffmann S. D. M. White, 2001, MNRAS, 320, 289-306,
  Preprint astro-ph/0005485
  
  

For all of the following images the credit should be Kauffmann, Colberg, Diaferio, and White, see references.
By clicking on the picture you can get the picture in its original size.

Pic.1 Projected dark matter distribution at z=3, 2, 1, and 0 (tauCDM)

ps format

Pic.2 Dark Matter at z=0 plus model galaxies formed at different epoch (tauCDM).
Top left panel only shows the galaxies which were formed at z>=3; top right panel shows the galaxies which were formed at z>=2; bottom left panel shows the galaxies which were formed at z>=1, and bottom right panel shows the galaxies which were formed at z>=0.

Pic.3 Dark Matter plus model galaxies at z=3, 2, 1, and 0 (tauCDM)
Galaxies are plotted at each redshift.

Pic.4 Dark Matter distribution of GIF boxes of four different cosmologies.
(Time sequence z=3, 2, 1, and 0)

Pic.5 A slice of thickness 8 Mpc/h through the whole simulation box (which is 85 Mpc/h on a side) would look like this. The colours now denote the B-V colours of the galaxies, ranging from red for ellipticals to blue for irregulars.

Pic.6 One of the clusters from the tauCDM simulation at z=0.
The size of the region shown is 21x21x8 Mpc/h.

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Last modified: Sat Mar 10 17:09:05 MET 2001 by WebMaster