A physical model for the evolving UV luminosity function of high
  redshift galaxies and their contribution to the cosmic reionization
  [Abridged] We present a physical model for the evolution of the ultraviolet
(UV) luminosity function (LF) of high-z galaxies taking into account in a
self-consistent way their chemical evolution and the associated evolution of
dust extinction. The model yields good fits of the UV and Lyman-alpha LFs at
z>~2. The weak evolution of both LFs between z=2 and z=6 is explained as the
combined effect of the negative evolution of the halo mass function, of the
increase with redshift of the star formation efficiency, and of dust
extinction. The slope of the faint end of the UV LF is found to steepen with
increasing redshift, implying that low luminosity galaxies increasingly
dominate the contribution to the UV background at higher and higher redshifts.
The observed range of UV luminosities at high-z implies a minimum halo mass
capable of hosting active star formation M_crit <~ 10^9.8 M_odot, consistent
with the constraints from hydrodynamical simulations. From fits of Lyman-alpha
LFs plus data on the luminosity dependence of extinction and from the measured
ratios of non-ionizing UV to Lyman-continuum flux density for samples of z=~3
Lyman break galaxies and Lyman-alpha emitters, we derive a simple relationship
between the escape fraction of ionizing photons and the star formation rate,
impling larger escape fraction for less massive galaxies. Galaxies already
represented in the UV LF (M_UV <~ -18) can keep the universe fully ionized up
to z=~6, consistent with (uncertain) data pointing to a rapid drop of the
ionization degree above z~6. On the other side, the electron scattering optical
depth, tau_es, inferred from CMB experiments favor an ionization degree close
to unity up to z=~9-10. Consistency with CMB data can be achieved if M_crit =~
10^8.5 M_odot, implying that the UV LFs extend to M_UV =~ -13, although the
corresponding tau_es is still on the low side of CMB-based estimates.
