Top panel: comparison between the dynamical mass M_dyn and the total mass content M_tot (=M_gas + M_* + M_darkmatter) for our SBs sample, color coded by their total attenuation A_V, tot. Bottom panel: diagram showing the square of the total FWHM velocity width as a function of M_tot/FWHM_radio, using the same color coding based on A_V, tot. On the y-axis, const = 1.3 × G/(4⟨sin²(i)⟩) groups the coefficients in Eq. (3) so as to facilitate comparison with the virialized case (1:1 relation, shown as a gray dotted line). The blue continuous line represents a linear fit to our sample, excluding galaxies with an upper limit on their radio size, while the blue shaded area shows the ±1σ limits of this best-fit relation. Both panels of the figure suggest that our galaxies may be approaching virialization, and more obscured starbursts are closer to the equilibrium.