Testing baryon-induced core formation in $\Lambda$CDM: A comparison of
  the DC14 and coreNFW dark matter halo models on galaxy rotation curves
  Recent cosmological hydrodynamical simulations suggest that baryonic
processes, and in particular supernova feedback after bursts of star formation,
can alter the structure of dark matter haloes and transform primordial cusps
into shallower cores. To assess whether this mechanism offers a solution to the
cusp-core controversy, simulated haloes must be compared to real dark matter
haloes inferred from galaxy rotation curves. For this purpose, two new dark
matter density profiles were recently derived from simulations of galaxies in
complementary mass ranges: the DC14 halo ($10^{10} < M_{\text{halo}}/M_{\odot}
< 8 \times 10^{11}$) and the coreNFW halo ($10^{7} < M_{\text{halo}}/M_{\odot}
< 10^{9}$). Both models have individually been found to give good fits to
observed rotation curves. For the DC14 model, however, the agreement of the
predicted halo properties with cosmological scaling relations was confirmed by
one study, but strongly refuted by another. A next question is whether the two
models converge to the same solution in the mass range where both should be
appropriate. To investigate this, we tested the DC14 and cNFW halo models on
the rotation curves of a selection of galaxies with halo masses in the range $4
\times 10^{9}$ - $7 \times 10^{10}$ $M_{\odot}$. We further applied the DC14
model to a set of rotation curves at higher halo masses, up to $9 \times
10^{11}$ $M_{\odot}$, to verify the agreement with the cosmological scaling
relations. We find that both models are generally able to reproduce the
observed rotation curves, in line with earlier results, and the predicted dark
matter haloes are consistent with the cosmological $c-M_{\text{halo}}$ and
$M_{*}-M_{\text{halo}}$ relations. The DC14 and cNFW models are also in fairly
good agreement with each other, even though DC14 tends to predict slightly less
extended cores and somewhat more concentrated haloes than cNFW.
