The Effect of the Angular Momentum in the Formation and Evolution of Low
  Surface Brightness Galaxies
  Using observed data from the literature, we compare in one single publication
the angular momentum (AM) of low surface brightness galaxies (LSBGs), with that
of high surface brightness galaxies (HSBGs), a comparison that either is
currently spread across many unconnected references, or simply does not exist.
Partly because of the subject, this has received little attention outside the
realm of simulations. We use previous results of the stellar specific AM
$j_{*}$ from the SPARC database containing Spitzer 3.6 $\mu$m photometry and
accurate H I rotation curves from Lelli et al. using a sample of 38 LSBGs and
82 HSBGs. We do this with the objective of comparing both galaxy populations,
finding that LSBGs are higher in the Fall relation by about 0.174 dex.
Additionally, we apply and test different masses and formation models to
estimate the spin parameter $\lambda$, which quantifies the rotation obtained
from the tidal torque theory, finding no clear evidence of a difference in the
spin of LSBGs and HSBGs under a classic disk formation model that assumes the
ratio ($f_{j}$) between $j_{*}$ and the specific AM of the halo is $\sim 1$. In
another respect, by using the biased collapse model, where $f_{j}$ depends on
the star formation efficiency, it was found that LSBGs clearly show higher spin
values, having an average spin of $\sim 2$ times the average spin of HSBGs.
This latter result is consistent with those obtained from simulations by
Dalcanton et al.
