IGM metal enrichment through dust sputtering

We study the motion of dust grains into the Intergalactic Medium (IGM) around redshift z = 3, to test the hypothesis that grains can efficiently pollute the gas with metals through sputtering. We use the results available in the literature for radiation-driven dust ejection from galaxies as initial conditions, and follow the motion onward. Via this mechanism, grains are ejected into the IGM with velocities > 100 km s; as they move supersonically, grains can be efficiently eroded by non-thermal sputtering. However, Coulomb and collisional drag forces effectively reduce the charged grain velocity. Up-to-date sputtering yields for graphite and silicate (olivine) grains have been derived using the code TRIM, for which we provide analytic fits. After training our method on a homogeneous density case, we analyze the grain motion and sputtering in the IGM density field as derived from a ΛCDM cosmological simulation at z = 3.27. We found that only large (a & 0.1-μm) grains can travel up to considerable distances (few ×100 kpc physical) before being stopped. Resulting metallicities show a well defined trend with overdensity δ. The maximum metallicities are reached for 10 < δ < 100 (corresponding to systems, in QSO absorption spectra, with 14.5 < logN(H i) < 16). However the distribution of sputtered metals is very inhomogeneous, with only a small fraction of the IGM volume polluted by dust sputtering (filling factors of 18 per cent for Si and 6 per cent for C). For the adopted size distribution, grains are never completely destroyed; nevertheless, the extinction and gas photo-electric heating effects due to this population of intergalactic grains are well below current detection limits.