Strongly Coupled Dark Energy Cosmologies: preserving LCDM success and
  easing low scale problems II - Cosmological simulations
  In this second paper we present the first Nbody cosmological simulations of
strongly coupled Dark Energy models (SCDEW), a class of models that alleviates
theoretical issues related to the nature of dark energy. SCDEW models assume a
strong coupling between Dark Energy (DE) and an ancillary Cold Dark Matter
(CDM) component together with the presence of an uncoupled Warm Dark Matter
component. The strong coupling between CDM and DE allows us to preserve small
scale fluctuations even if the warm particle is quite light ($\approx 100$ eV).
Our large scale simulations show that, for $10^{11}<M/M_\odot<10^{14}$, SCDEW
haloes exhibit a number density and distribution similar to a standard Lambda
Cold Dark Matter (LCDM) model, even though they have lower concentration
parameters. High resolution simulation of a galactic halo ($M\sim 10^{12}
M_{\odot} $) shows $\sim 60\%$ less substructures than its LCDM counterpart,
but the same cuspy density profile. On the scale of galactic satellites ($M\sim
10^{9} M_{\odot}$) SCDEW haloes dramatically differ from LCDM. Due to the high
thermal velocities of the WDM component they are almost devoid of any
substructures and present strongly cored dark matter density profiles. These
density cores extend for several hundreds of parsecs, in very good agreement
with Milky Way satellites observations. Strongly coupled models, thanks to
their ability to match observations on both large and small scales might
represent a valid alternative to a simple LCDM model.
