The relation between specific baryon angular momentum and mass for a
  sample of nearby low-mass galaxies with resolved HI kinematics
  This paper investigates the relationship between specific baryon angular
momentum $j_\mathrm{b}$ and baryon mass $M_\mathrm{b}$ for a sample of nearby
late-type galaxies with resolved HI kinematics. This work roughly doubles the
number of galaxies with $M_\mathrm{b} \lesssim 10^{10}$ $M_{\odot}$ used to
study the $j_\mathrm{b} - M_\mathrm{b}$ relation. Most of the galaxies in the
sample have their baryon mass dominated by their gas content, thereby offering
$j_\mathrm{b}$ and Mb measures that are relatively unaffected by uncertainties
arising from the stellar mass-to-light ratio. Measured HI surface density
radial profiles together with optical and rotation curve data from the
literature are used to derive a best-fit relation given by
$j_\mathrm{b}=qM_\mathrm{b}^{\alpha}$, with $\alpha=0.62\pm 0.02$ and
$\log_{10}q=-3.35\pm 0.25$. This result is consistent with the
$j_\mathrm{b}\propto M_\mathrm{b}^{2/3}$ relation that is theoretically
expected and also measured by Obreschkow & Glazebrook (2014) for their full
sample of THINGS spiral galaxies, yet differs to their steeper relation found
for subsets with fixed bulge fraction. The 30 arcsec spatial resolution of the
HI imaging used in this study is significantly lower than that of the THINGS
imaging used by Obreschkow & Glazebrook (2014), yet the results presented in
this work are clearly shown to contain no significant systematic errors due to
the low-resolution imaging.
