The evolution of H I and C IV quasar absorption line systems at 1.9 < z < 3.2

Abstract

We have investigated the distribution and evolution of ~3100 intergalactic neutral hydrogen (H i) absorbers with H I column densities log N_{H I} = [12.75,17.0] at 1.9 < z < 3.2, using 18 high resolution, high signal-to-noise quasar spectra obtained from the ESO VLT/UVES archive. We used two sets of Voigt profile fitting analysis, one including all the available high-order Lyman lines to obtain reliable H I column densities of saturated lines, and another using only the Lyα transition. There is no significant difference between the Lyα-only fit and the high-order Lyman fit results. Combining our Lyα-only fit results at 1.7 < z < 3.6 with high-quality literature data, the mean number density at 0 < z < 4 is not well described by a single power law and strongly suggests that its evolution slows down at z ≤ 1.5 at the high and low column density ranges. We also divided our entire H I absorbers at 1.9 < z < 3.2 into two samples, the unenriched forest and the C IV-enriched forest, depending on whether H I lines are associated with C IV at log N_{C IV} ≥ 12.2 within a given velocity range. The entire H I column density distribution function (CDDF) can be described as the combination of these two well-characterised populations which overlap at log N_{H I} ~ 15. At log N_{H I} ≤ 15, the unenriched forest dominates, showing a similar power-law distribution to the entire forest. The C IV-enriched forest dominates at log N_{H I} ≥ 15, with its distribution function as ∝N_{H I}^~-1.45. However, it starts to flatten out at lower N_{H I}, since the enriched forest fraction decreases with decreasing N_{H I}. The deviation from the power law at log N_{H I} = [14,17] shown in the CDDF for the entire H I sample is a result of combining two different H I populations with a different CDDF shape. The total H I mass density relative to the critical density is Ω_{H I} ~ 1.6 × 10^-6 h^-1, where the enriched forest accounts for ~40% of Ω_{H I}.

The data used in this study are taken from the ESO archive for the UVES at the VLT, ESO, Paranal, Chile.Appendix A is available in electronic form at http://www.aanda.org