Connecting cosmological accretion to strong Lyman-alpha absorbers
  We present an analytical model for the cosmological accretion of gas onto
dark matter halos, based on a similarity solution applicable to spherical
systems. Performing simplified radiative transfer, we compute how the accreting
gas turns increasingly neutral as it self-shields from the ionising background,
and obtain the column density, $N_{\rm HI}$, as a function of impact parameter.
The resulting column-density distribution function (CDDF) is in excellent
agreement with observations. The analytical expression elucidates (1) why halos
over a large range in mass contribute about equally to the CDDF as well as (2)
why the CDDF evolves so little with redshift in the range $z=2\rightarrow 5$.
We show that the model also predicts reasonable DLA line-widths ($v_{90}$),
bias and molecular fractions. Integrating over the CDDF yields the mass density
in neutral gas, $\Omega_{\rm HI}$, which agrees well with observations.
$\Omega_{\rm HI}(z)$ is nearly constant even though the accretion rate onto
halos evolves. We show that this occurs because the fraction of time that the
inflowing gas is neutral depends on the dynamical time of the halo, which is
inversely proportional to the accretion rate. Encapsulating results from
cosmological simulations, the simple model shows that most Lyman-limit system
and damped Lyman-alpha absorbers are associated with the cosmological accretion
of gas onto halos.
