Volume 458, Number 2, November I 2006
|Page(s)||427 - 439|
|Published online||12 September 2006|
The evolution of Lyman α absorbers in the redshift range
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [ejanknecht;dreimers]@hs.uni-hamburg.de
2 Departamento de Astronomia, Universidad de Chile, Casilla 36, Santiago, Chile e-mail: email@example.com
3 Center for Astrophysics and Space Sciences, University of California, San Diego, MS 0424, La Jolla, CA 92093-0424, USA e-mail: firstname.lastname@example.org
Accepted: 28 July 2006
We investigate the evolution and the statistical properties of the Ly α absorbers of the intergalactic medium (IGM) in the largely unexplored redshift range . We use high-resolution () UV (STIS) and optical (VLT/UVES and Keck/HIRES) spectra of nine bright quasars with . The Ly α lines detected in the lines of sight (LOS) towards these quasars are evaluated with a software package which determines simultaneously the quasar continuum and the line profiles. The main results for the combined Ly α line sample are summarized as follows: 1. The evolution of the number density of the absorbers can be described by the power law . The number density of the low column density lines ( cm-2) decreases with decreasing z with in the interval . A comparison with results at higher redshifts shows that it is decelerated in the explored redshift range and turns into a flat evolution for . The stronger absorbers ( cm-2) thin out faster (). The break in their evolution predicted for cannot be seen down to . On the other hand, a comparison with values from the literature for the local number density gives a hint that this break occurs at lower redshift. 2. The distribution of the column densities of the absorbers is complete down to cm-2. It can be approximated by a single power law with the exponent over almost three orders of magnitude. β is redshift independent. 3. The Ly α lines with lower column densities as well as the higher column density lines show marginal clustering with a significance over short distances ( km s-1 and km s-1, respectively). We do not see any difference in the clustering with either column density or redshift. 4. The distribution of the Doppler parameters has a mean value of km s-1. This value is typical for the analyzed region. It does not change significantly with z.
Key words: cosmology: observations / intergalactic medium
© ESO, 2006
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