Kinematics and star formation activity in the z=2.03954 damped Lyman-alpha system towards PKS 0458-020

Details Kinematics and star formation activity in the z=2.03954 damped Lyman-alpha system towards PKS 0458-020 Kinematics and star formation activity in the z=2.03954 damped Lyman-alpha system towards PKS 0458-020

2005-12-05

arxiv.org/abs/astro-ph/0512118v1

Astron.Astrophys. 449 (2006) 33-39

Astronomy and Astrophysics

Astrophysics

accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20053910

We present UVES observations of the log N(HI)= 21.7 damped Lyman-alpha system at z=2.03954 towards the quasar PKS 0458-020. HI Lyman-alpha emission is detected in the center of the damped Lyman-alpha absorption trough. Metallicities are derived for MgII, SiII, PII, CrII, MnII, FeII and ZnII and are found to be -1.21\pm0.12, -1.28\pm0.20, -1.54\pm0.11, -1.66\pm0.10, -2.05\pm0.11, -1.87\pm0.11, -1.22\pm0.10, respectively, relative to solar. The depletion factor is therefore of the order of [Zn/Fe]=0.65. We observe metal absorption lines to be blueshifted compared to the Lyman-alpha emission up to a maximum of 100 and 200 km/s for low and high-ionization species respectively. This can be interpreted either as the consequence of rotation in a large (~7kpc) disk or as the imprint of a galactic wind. The star formation rate (SFR) derived from the Lyman-alpha emission, 1.6 solar masses/yr, is compared with that estimated from the observed CII* absorption. No molecular hydrogen is detected in our data, yielding a molecular fraction f<-6.52. This absence of H2 can be explained as the consequence of a high ambient UV flux which is one order of magnitude larger than the radiation field in the ISM of our Galaxy and originates in the observed emitting region.

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