Simulating cosmic metal enrichment by the first galaxies
  We study cosmic metal enrichment via AMR hydrodynamical simulations in a (10
Mpc/h)$^3$ volume following the Pop III-Pop II transition and for different Pop
III IMFs. We have analyzed the joint evolution of metal enrichment on galactic
and intergalactic scales at z=6 and z=4. Galaxies account for <9% of the
baryonic mass; the remaining gas resides in the diffuse phases: (a) voids, i.e.
regions with extremely low density ($\Delta$<1), (b) the true intergalactic
medium (IGM, 1<$\Delta$<10) and (c) the circumgalactic medium (CGM,
10<$\Delta<10^{2.5}$), the interface between the IGM and galaxies. By z=6 a
galactic mass-metallicity relation is established. At z=4, galaxies with a
stellar mass $M_*=10^{8.5}M_\odot$ show log(O/H)+12=8.19, consistent with
observations. The total amount of heavy elements rises from
$\Omega^{SFH}_Z=1.52\, 10^{-6}$ at z=6 to 8.05 $10^{-6}$ at z=4. Metals in
galaxies make up to ~0.89 of such budget at z=6; this fraction increases to
~0.95 at z=4. At z=6 (z=4) the remaining metals are distributed in
CGM/IGM/voids with the following mass fractions: 0.06/0.04/0.01
(0.03/0.02/0.01). Analogously to galaxies, at z=4 a density-metallicity
($\Delta$-Z) relation is in place for the diffuse phases: the IGM/voids have a
spatially uniform metallicity, Z~$10^{-3.5}$Zsun; in the CGM Z steeply rises
with density up to ~$10^{-2}$Zsun. In all diffuse phases a considerable
fraction of metals is in a warm/hot (T>$10^{4.5}$K) state. Due to these
physical conditions, CIV absorption line experiments can probe only ~2% of the
total carbon present in the IGM/CGM; however, metal absorption line spectra are
very effective tools to study reionization. Finally, the Pop III star formation
history is almost insensitive to the chosen Pop III IMF. Pop III stars are
preferentially formed in truly pristine (Z=0) gas pockets, well outside
polluted regions created by previous star formation episodes.
