Angular momentum of dwarf galaxies
  Mass and specific angular momentum are two fundamental physical parameters of
galaxies. We present measurements of the baryonic mass and specific angular
momentum of 11 void dwarf galaxies derived from neutral hydrogen (H{\sc i})
synthesis data. Rotation curves were measured using 3D and 2D tilted ring
fitting routines, and the derived curves generally overlap within the error
bars, except in the central regions where, as expected, the 3D routines give
steeper curves. The specific angular momentum of void dwarfs is found to be
high compared to an extrapolation of the trends seen for higher mass bulge-less
spirals, but comparable to that of other dwarf irregular galaxies that lie
outside of voids. As such, our data show no evidence for a dependence of the
specific angular momentum on the large scale environment. Combining our data
with the data from the literature, we find a baryonic threshold of $\sim
10^{9.1}~M_{\odot}$ for this increase in specific angular momentum.
Interestingly, this threshold is very similar to the mass threshold below which
the galaxy discs start to become systematically thicker. This provides
qualitative support to the suggestion that the thickening of the discs, as well
as the increase in specific angular momentum, are both results of a common
physical mechanism, such as feedback from star formation. Quantitatively,
however, the amount of star formation observed in our dwarfs appears
insufficient to produce the observed increase in specific angular momentum. It
is hence likely that other processes, such as cold accretion of high angular
momentum gas, also play a role in increasing the specific angular momentum.
