to dark matter halos with the virial quantities presented in table \[table:table1\] are listed in table \[table:table2\].

The previously mentioned code can generate a disk component of a galaxy according to the cylindrical spatial distribution: $$\rho_{stars}\left(r,z\right) = \rho_{0} \exp \left( -\frac{r}{R_d} \right) \left[ sech \left( \frac{z}{z_c} \right) \right] ^2,$$ and cylindrical distribution of the radial dispersion:

$$\sigma_r(r) = \sigma_{r0} \left( \exp \left( - \frac{r}{R_d} \right) \right)^{1/2}.$$

The reader who is interested in more details on how the code constructs the galactic model is referred to the publication [@2008ApJ...679.1239W].

There are free parameters that have to be set using educated guesses based on available constraints on galactic structure at low mass scales. Most importantly, the mass of the stellar disk $M_d$ for each object is $1.2 \times 10^{-3}$ of its virial mass Such ratio is chosen to reflect the stellar-to-halo mass ratio, $M_{\star}/M_{vir}$, inferred from the abundance matching analysis extrapolated to lower masses ([@2013ApJ...770...57B]). Past simulations of disk galaxy formation presented in the [@2007MNRAS.382.1187K] paper associate to objects with maximum circular velocities in the 24-53 km $s^{-1}$range, scale height values in the 0.08-0.18 kpc range. Considering the previously mentioned results the values of the scale heights of all the objects is 