  We use a sample of galaxies from the Sloan Digital Sky Survey (SDSS) to
search for correlations between the $\lambda$ spin parameter and the
environment and mass of galaxies. In order to calculate the total value of
$\lambda$ for each observed galaxy, we employed a simple model of the dynamical
structure of the galaxies which allows a rough estimate of the value of
$\lambda$ using only readily obtainable observables from the luminous galaxies.
Use of a large volume limited sample (upwards of 11,000) allows reliable
inferences of mean values and dispersions of $\lambda$ distributions. We find,
in agreement with some N-body cosmological simulations, no significant
dependence of $\lambda$ on the environmental density of the galaxies. For the
case of mass, our results show a marked correlation with $\lambda$, in the
sense that low mass galaxies present both higher mean values of $\lambda$ and
associated dispersions, than high mass galaxies. This last direct empirical
result, at odds with expectations from N-body cosmological simulations,
provides interesting constrain on the mechanisms of galaxy formation and
acquisition of angular momentum, a valuable test for cosmological models.
