  We present a new method to remove the impact of random and small-scale
non-circular motions from HI velocity fields in galaxies in order to better
constrain the dark matter properties for these objects. This method extracts
the circularly rotating velocity components from the HI data cube and condenses
them into a so-called bulk velocity field. We derive high-resolution rotation
curves of IC 2574 and NGC 2366 based on bulk velocity fields derived from The
HI Nearby Galaxy Survey (THINGS) obtained at the VLA. The bulk velocity field
rotation curves are significantly less affected by non-circular motions and
constrain the dark matter distribution in our galaxies, allowing us to address
the discrepancy between the inferred and predicted dark matter distribution in
galaxies (the "cusp/core" problem). Spitzer Infrared Nearby Galaxies Survey
(SINGS) 3.6 micron data as well as ancillary optical information, are used to
separate the baryons from the total matter content. Using stellar population
synthesis models, assuming various sets of metallicity and star formation
histories, we compute stellar mass-to-light ratios for the 3.6 and 4.5 micron
bands. Using our predicted value for the 3.6 micron stellar mass-to-light
ratio, we find that the observed dark matter distributions of IC 2574 and NGC
2366 are inconsistent with the cuspy dark matter halo predicted by LCDM models,
even after corrections for non-circular motions. This result also holds for
other assumptions about the stellar mass-to-light ratio. The distribution of
dark matter within our sample galaxies is best described by models with a
kpc-sized constant-density core.
