Self-gravitating equilibrium models of dwarf galaxies and the minimum
  mass for star formation
  We construct a series of model galaxies in rotational equilibrium consisting
of gas, stars, and a fixed dark matter (DM) halo and study how these
equilibrium systems depend on the mass and form of the DM halo, gas
temperature, non-thermal and rotation support against gravity, and also on the
redshift of galaxy formation. For every model galaxy we find the minimum gas
mass M_g^min required to achieve a state in which star formation (SF) is
allowed according to contemporary SF criteria. The obtained M_g^min--M_DM
relations are compared against the baryon-to-DM mass relation M_b--M_DM
inferred from the \LambdaCDM theory and WMAP4 data. Our aim is to construct
realistic initial models of dwarf galaxies (DGs), which take into account the
gas self-gravity and can be used as a basis to study the dynamical and chemical
evolution of DGs. Rotating equilibria are found by solving numerically the
steady-state momentum equation for the gas component in the combined
gravitational potential of gas, stars, and DM halo using a forward substitution
procedure. We find that for a given M_DM the value of M_g^min depends crucially
on the gas temperature T_g, gas spin parameter \alpha, degree of non-thermal
support \sigma_eff, and somewhat on the redshift for galaxy formation z_gf.
Depending on the actual values of T_g, \alpha, \sigma_eff, and z_gf, model
galaxies may have M_g^min that are either greater or smaller than M_b. Galaxies
with M_DM \ga 10^9 M_sun are usually characterized by M_g^min \la M_b, implying
that SF in such objects is a natural outcome as the required gas mass is
consistent with what is available according to the \LambdaCDM theory. On the
other hand, models with M_DM \la 10^9 M_sun are often characterized by M_g^min
>> M_b, implying that they need much more gas than available to achieve a state
in which SF is allowed. Abridged.
