Patrick Valageas web page

At large scales the gas follows the density fluctuations of the dark matter. The gravitational instability which governs the dynamics builds a complex network of a wide variety of structures: voids, filaments, dense and massive halos (see Gravitational dynamics). At small scales the gas within dense objects can cool by radiating its energy away. This implies a further collapse of the gas which can eventually form stars and galaxies. Understanding and modeling the formation of galaxies is a very difficult problem because of the broad range of physical processes and scales which need to be taken into account.

Articles:

• 2001, A&A, 366, 363
  An analytical description of the relationship between the distributions of dark matter matter and baryons: bias of various objects (clusters, galaxies, quasars, Lyman-alpha clouds).
  
• 2000, A&A, 359, 821
  A compared study of clusters and groups of galaxies, galaxies and quasars. Comparison of analytical models with observations.
  
• 1999, A&A, 345, 329
  An analytical model for the formation and evolution of galaxies.