Gas surface densities (left column), Toomre Q parameters (middle column), and rotation velocities (right column) of self-gravitating (steady-state) gaseous disk hosted by quasi-isothermal DM halos with four masses M_DM as indicated in the right-hand column. The spatially uniform gas temperature and the spin parameter are set to T_g = 10⁴ K and α = 0.9, respectively. The horizontal dotted lines mark the adopted critical surface density for star formation Σ_c = 5   M_⊙ pc² (left column) and the critical Toomre parameter Q_cr for gravitational stability (middle column). For every value of M_DM, five models with different values of the seed density n_0,0 = 25.0, 5.0, 1.0, 0.1, and 0.01 cm^-3 from the uppermost to the lowermost line are considered. Higher n_0,0 produce models with higher gas surface densities in the inner regions. The models that are susceptible to star formation according to the adopted star formation criteria are marked with red thick lines and the gas mass with number density higher than a critical value of 1.0 cm^-3 is indicated in the left column for models plotted with solid red lines.