  We study 379 central and 159 satellite early-type galaxies with
two-dimensional kinematics from the integral-field survey Mapping Nearby
Galaxies at APO (MaNGA) to determine how their angular momentum content depends
on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we
identify central and satellite galaxies in groups with halo masses in the range
10^12.5 h^-1 M_sun < M_200b < 10^15 h^-1 M_sun. As in previous work, we see a
sharp dependence on stellar mass, in the sense that ~ 70% of galaxies with
stellar mass M_* > 10^11 h^-2 M_sun tend to have very little rotation, while
nearly all galaxies at lower mass show some net rotation. The ~ 30% of
high-mass galaxies that have significant rotation do not stand out in other
galaxy properties except for a higher incidence of ionized gas emission. Our
data are consistent with recent simulation results suggesting that major
merging and gas accretion have more impact on the rotational support of
lower-mass galaxies. When carefully matching the stellar mass distributions, we
find no residual differences in angular momentum content between satellite and
central galaxies at the 20\% level. Similarly, at fixed mass, galaxies have
consistent rotation properties across a wide range of halo mass. However, we
find that errors in classification of centrals and satellites with group
finders systematically lowers differences between satellite and central
galaxies at a level that is comparable to current measurement uncertainties. To
improve constraints, the impact of group finding methods will have to be
forward modeled via mock catalogs.
