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We present UVES observations of the log N(HI)= 21.7 damped Lyman-alpha systemat z=2.03954 towards the quasar PKS 0458-020. HI Lyman-alpha emission isdetected in the center of the damped Lyman-alpha absorption trough.Metallicities are derived for MgII, SiII, PII, CrII, MnII, FeII and ZnII andare 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. Thedepletion factor is therefore of the order of [Zn/Fe]=0.65. We observe metalabsorption lines to be blueshifted compared to the Lyman-alpha emission up to amaximum 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 comparedwith that estimated from the observed CII* absorption. No molecular hydrogen isdetected in our data, yielding a molecular fraction f<-6.52. This absence of H2can be explained as the consequence of a high ambient UV flux which is oneorder of magnitude larger than the radiation field in the ISM of our Galaxy andoriginates in the observed emitting region.Comment: accepted for publication in A&

Kinematics and star formation activity in the z$\mathsf{_{abs}}$ = 2.03954 damped Lyman-$\mathsf{\alpha}$ system towards PKS 0458–020