  We build a volume-limited sample of galaxies derived from the SDSS-DR7 to
characterize several physical properties of the dark matter halos where LSB
galaxies reside. Using an observational proxy for the assembly time, we found
that LSB galaxies assembly half of their total halo mass later than HSB ones,
reinforcing the idea of them being unevolved systems. We use 5 different
methods to estimate the total halo mass, finding that the total stellar-to-halo
mass ratio is up to 22% lower in LSB galaxies. Finally, in order to estimate
the spin parameter, we use a bulge+disk decomposition to obtain the specific
angular momentum $j_*$ of the galaxy, a Tully-Fisher relation to estimate the
rotation velocity of the disk, and the 5 different estimations of the halo mass
to calculate the spin parameter. We found that the spin of LSB galaxies is 1.2
to 2 times higher than for HSB ones. We compare these results with a control
sample that includes kinematic information, taken from the ALFALFA $\alpha$.100
galaxy catalog, allowing us to measure directly the rotation velocity of the
disk. The trends in the values of $j_*$ and $\lambda$ are similar to the
volume-limited sample.
