The imprint of dark matter haloes on the size and velocity dispersion
  evolution of early-type galaxies
  Early-type galaxies (ETGs) are observed to be more compact, on average, at $z
\gtrsim 2$ than at $z\simeq 0$, at fixed stellar mass. Recent observational
works suggest that such size evolution could reflect the similar evolution of
the host dark matter halo density as a function of the time of galaxy
quenching. We explore this hypothesis by studying the distribution of halo
central velocity dispersion ($\sigma_0$) and half-mass radius ($r_{\rm h}$) as
functions of halo mass $M$ and redshift $z$, in a cosmological $\Lambda$-CDM
$N$-body simulation. In the range $0\lesssim z\lesssim 2.5$, we find
$\sigma_0\propto M^{0.31-0.37}$ and $r_{\rm h}\propto M^{0.28-0.32}$, close to
the values expected for homologous virialized systems. At fixed $M$ in the
range $10^{11} M_\odot \lesssim M\lesssim 5.5 \times 10^{14} M_\odot$ we find
$\sigma_0\propto(1+z)^{0.35}$ and $r_{\rm h}\propto(1+z)^{-0.7}$. We show that
such evolution of the halo scaling laws is driven by individual haloes growing
in mass following the evolutionary tracks $\sigma_0\propto M^{0.2}$ and $r_{\rm
h}\propto M^{0.6}$, consistent with simple dissipationless merging models in
which the encounter orbital energy is accounted for. We compare the $N$-body
data with ETGs observed at $0\lesssim z\lesssim3$ by populating the haloes with
a stellar component under simple but justified assumptions: the resulting
galaxies evolve consistently with the observed ETGs up to $z \simeq 2$, but the
model has difficulty reproducing the fast evolution observed at $z\gtrsim 2$.
We conclude that a substantial fraction of the size evolution of ETGs can be
ascribed to a systematic dependence on redshift of the dark matter haloes
structural properties.
