Hot Baryons and the Distribution of Metals in the Intergalactic Medium

We use the observed number and column-density distributions of intergalactic O VI absorbers to constrain the distribution of metals in the low-redshift intergalactic medium (IGM). In this simple model the metals in the O VI absorbers are assumed to be produced in and propagated from lowredshift galaxies drawn from a real sample, in this case the Sloan Digital Sky Survey (SDSS). This model can explain the observed dN/dz of metals seen in O VI absorbers if these metals are dispersed out to ∼ 200 kpc by galaxies down to L ∼ 0.01 − 0.1L∗r. Massive galaxies (L ∼ L ∗ r) by themselves cannot provide the necessary enrichment unless they can enrich volumes out to & 0.5 − 1 Mpc. Alternatively, our model allows an estimate of the fraction of O VI absorbers directly caused by galaxies rather than hot IGM. With this assumption we explore the possible connections between the intergalactic O VI absorbers and the known populations of highly-ionized high-velocity clouds (HVCs) surrounding the Milky Way. Our model predicts that more sensitive, complete surveys optimized to uncover weaker O VI absorbers will find the tentative turnover below logN(O VI) ∼ 13.5 to be a real effect resulting from the apparently limited volumes over which galaxies can enrich the IGM. If so, it would indicate that metals are not as widespread throughout the low-density IGM as they are assumed to be in cosmological simulations of the WHIM. Subject headings: intergalactic medium — quasars: absorption lines