  The formation of the disk and feedback from supernova winds impacts the
distribution of dark matter in galaxies. Recently, Di Cintio et al. (2014b)
characterized the halo response from baryonic processes in hydrodynamical
simulations via a dependence on the ratio of stellar-to-halo mass
($M_{\star}/M_{{\rm halo}}$). The (stellar) mass dependent halo profile links
together the local and global properties of the halo (e.g. inner slope and
$M_{{\rm halo}}$) which allows for measurements of $M_{{\rm halo}}$ without
virial tracers. We compile a large sample of rotation curves from the
literature to test this halo profile. We find that this halo profile can
explain rotation curve observations over a wide range of $M_{\star}$. However,
the global results from our sample are inconsistent with a $\Lambda$ cold dark
matter universe. We do not find the expected correlation between the halo
concentration and $M_{{\rm halo}}$ and there is significantly larger scatter
than expected. Furthermore, a large portion of galaxies below $M_{\star} \sim
10^{9}\,M_{\odot}$ are found to be hosted by smaller halos than expectations
from the abundance matching technique. We find our results are robust to
statistical priors and systematic effects such as inclination angle, asymmetric
drift correction, data source, and uncertainties in stellar mass-to-light
ratios. This suggests either a mischaracterization of the halo response due to
baryonic processes or additional non-standard dark matter physics.
