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 H i 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 M _ { \mathrm { b } } measures that are relatively unaffected by uncertainties arising from the stellar mass-to-light ratio .
Measured H i 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 \citet OG14 for their full sample of THINGS spiral galaxies , \textcolor blackyet differs to their steeper relation found for subsets with fixed bulge fraction .
The 30 arcsec spatial resolution of the H i imaging used in this study is significantly lower than that of the THINGS imaging used by \citet OG14 , \textcolor blackyet the results presented in this work are clearly shown to contain no significant systematic errors due to the low-resolution imaging .