The evolution of neutral gas in damped Lyman α systems from the XQ-100 survey. Issue 4 (23rd January 2016)

• Record Type: Journal Article
• Authors: Sánchez-Ramírez, R.; Ellison, S. L.; Prochaska, J. X.; Berg, T. A. M.; López, S.; D'Odorico, V.; Becker, G. D.; Christensen, L.; Cupani, G.; Denney, K. D.; Pâris, I.; Worseck, G.; Gorosabel, J.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 456:Issue 4(2016)
• Page Start: 4488
• Page End: 4505
• Publication Date: 2016-01-23
• Subjects: galaxies: evolution -- galaxies: formation -- quasars: absorption lines -- cosmology: observations; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stv2732
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We present a sample of 38 intervening damped Lyman α (DLA) systems identified towards 100 z > 3.5 quasars, observed during the XQ-100 survey. The XQ-100 DLA sample is combined with major DLA surveys in the literature. The final combined sample consists of 742 DLAs over a redshift range approximately 1.6 < z abs < 5.0. We develop a novel technique for computing $\Omega _{\rm H\, {\small I}}^{\rm DLA}$ as a continuous function of redshift, and we thoroughly assess and quantify the sources of error therein, including fitting errors and incomplete sampling of the high column density end of the column density distribution function. There is a statistically significant redshift evolution in $\Omega _{\rm H\, \small {I}}^{\rm DLA}$ (≥3σ) from z ∼ 2 to z ∼ 5. In order to make a complete assessment of the redshift evolution of $\Omega _{\rm H\, \small {I}}$, we combine our high-redshift DLA sample with absorption surveys at intermediate redshift and 21-cm emission line surveys of the local universe. Although $\Omega _{\rm H\, \small {I}}^{\rm DLA}$, and hence its redshift evolution, remains uncertain in the intermediate-redshift regime (0.1 < z abs < 1.6), we find that the combination of high-redshift data with 21-cm surveys of the local universe all yield a statistically significant evolution in $\Omega _{\rm H\, \small {I}}$ from z ∼ 0 to z ∼ 5 (≥3σ). Despite its statistical significance, the magnitude of the evolution is small: a linear regression fit between $\Omega _{\rm H\, \small {I}}$ and z yields a typical slope of ∼0.17 × 10 −3, corresponding to a factor of ∼4 decrease in $\Omega _{\rm H\, \small {I}}$ between z = 5 and z = 0.