The Rise of Dwarfs and the Fall of Giants: Galaxy Formation Feedback   Signatures in the Halo Satellite Luminosity Function
  The observed luminosity function (LF) of satellite galaxies shows several interesting features that require a better understanding of gas-thermodynamic processes and feedback effects related to reionization and galaxy formation. In galaxy clusters, the abundance of dwarf galaxies is in good agreement with the expectation based on the subhalo mass function, whereas in galaxy groups, the relatively small abundance of dwarfs conflicts with theoretical expectations. In all halo systems, there is a dip in the abundance of galaxies with luminosities in the range ~ 2x10^8 L_sun to 10^10 L_sun, corresponding to subhalo mass scales between ~ 5x10^10 M_sun to few times 10^11 M_sun. Photoionization from reionization has been used to explain statistics of the dwarf population, with larger systems forming prior to, and smaller systems forming subsequent to, reionization. The observed dip in the LF is an imprint of small dwarf galaxies (<2x10^8 L_sun) that formed prior to reionization. The galactic winds powered by supernovae in these dwarf galaxies propagate energy and metals to large distances such that the intergalactic medium is uniformly enriched to a level of 10^-3 zsun, as observed in the low-redshift Ly-alpha forest. The associated energy related to this metallicity raises the intergalactic medium temperature and the Jeans mass to a range 10^10-10^11 M_sun at z ~ 3.4-6.0. Because the epoch of nonlinearity for halos in this mass range is at z > 3.4-4.4, their gas content, hence star formation, is greatly suppressed on average and leads to a dip in the observed LF at $z=0$. Larger halos (M > 10^11 M_sun), becoming nonlinear at z < 3.4-4.4, have masses topping the Jeans mass, where subhalo mass function based LF is again in agreement with observations. 
Asantha Cooray, Renyue Cen