The sources of intergalactic metals

We study the clustering properties of metals in the intergalactic medium (IGM) as traced by 619 CIV and 81 Si IV absorption components with N >= 10(12) cm(-2) and 316 MgII and 82 Fe II absorption components with N >= 10(11.5) cm(-2) in 19 high signal-to-noise ratio (60 - 100 pixel(-1)), high-resolution (R = 45 000) quasar spectra. C IV and Si IV trace each other closely and their line-of-sight correlation functions xi(v) exhibit a steep decline at large separations and a flatter profile below approximate to 150 km s(-1), with a large overall bias. These features do not depend on absorber column densities, although there are hints that the overall amplitude of xi C-IV (v) increases with time over the redshift range detected (1.5- 3). Carrying out a detailed smoothed particle hydrodynamic simulation ( 2 x 320(3), 57 Mpc(3) comoving), we show that the CIV correlation function cannot be reproduced by models in which the IGM metallicity is constant or a local function of overdensity (Z proportional to Delta(2/3)). However, the properties of xi(CIV)(v) are generally consistent with a model in which metals are confined within bubbles with a typical radius R-s about sources of mass >= M-s. We derive best-fitting values of R-s approximate to 2 comoving Mpc and M-s approximate to 10(12) M-. at z = 3. Our lower-redshift (0.5 - 2) measurements of the MgII and Fe II correlation functions also uncover a steep decline at large separations and a flatter profile at small separations, but the clustering is even higher than in the z = 1.5 - 3 measurements, and the turnover is shifted to somewhat smaller distances, approximate to 75 km s(-1). Again, these features do not change with column density, but there are hints that the amplitudes of xi(MgII)( v) and xi(Fe II)( v) increase with time. We describe an analytic 'bubble' model for these species, which come from regions that are too compact to be accurately simulated numerically, deriving best-fitting values of R-s approximate to 2.4 Mpc and M-s approximate to 10(12) M-.. Equally good analytic fits to all four species are found in a similarly biased high-redshift enrichment model in which metals are placed within 2.4 comoving Mpc of M-s approximate to 3 x 10(9) sources at z = 7.5.