The Cusp/Core problem: supernovae feedback versus the baryonic clumps
  and dynamical friction model
  In the present paper, we compare the predictions of two well known mechanisms
considered able to solve the cusp/core problem (a. supernova feedback; b.
baryonic clumps-DM interaction) by comparing their theoretical predictions to
recent observations of the inner slopes of galaxies with masses ranging from
dSphs to normal spirals. We compare the $\alpha$-$V_{\rm rot}$ and the
$\alpha$-$M_{\ast}$ relationships, predicted by the two models with high
resolution data coming from \citep{Adams2014,Simon2005}, LITTLE THINGS
\citep{Oh2015}, THINGS dwarves \citep{Oh2011a,Oh2011b}, THINGS spirals
\citep{Oh2015}, Sculptor, Fornax and the Milky Way. The comparison of the
theoretical predictions with the complete set of data shows that the two models
perform similarly, while when we restrict the analysis to a smaller subsample
of higher quality, we show that the method presented in this paper (baryonic
clumps-DM interaction) performs better than the one based on supernova
feedback. We also show that, contrarily to the first model prediction, dSphs of
small mass could have cored profiles. This means that observations of cored
inner profiles in dSphs having a stellar mass $<10^6 M_{\odot}$ not necessarily
imply problems for the $\Lambda$CDM model.
