The VLT-UVES survey for molecular hydrogen in high-redshift damped Lyman-alpha systems: Physical conditions in the neutral gas

Abstract

We study the physical conditions in DLAs, using a sample of 33 systems toward 26 QSOs acquired for a recently completed survey of H_2 by Ledoux et al. (2003). We use the column densities of H_2 in different rotational levels, together with those of C I, C I*, C I**, C II* and singly ionized atomic species to discuss the kinetic temperature, the density of hydrogen and the electronic density in the gas together with the ambient UV radiation field. Detailed comparisons are made between the observed properties in DLAs, the interstellar medium (ISM) of the Galaxy, LMC and SMC. The mean kinetic temperature of the gas corresponding to DLA subcomponents in which H_2 absorption line is detected, derived from the ortho-to-para ratio (153+/-78 K), is higher than that measured in the ISM (77+/-17 K) and the Magellanic clouds (82+/-21 K). Typical pressure in these components (corresponding to T = 100-300 K and n = 10-200 cm^-3), measured using C I fine-structure excitation, are higher than what is measured along ISM sightlines. This is consistent with the corresponding higher values for N(H_2,J=2)/N(H_2,J=0) seen in DLAs. From the column densities of the high-J rotational levels, we derive that the typical radiation field in the H_2 bearing components is of the order of or slightly higher than the mean UV field in the Galactic ISM. Determination of electron density in the gas with H_2 and C I show the ionization rate is similar to that of a cold neutral medium (CNM) in a moderate radiation field. This, together with the fact that we see H_2 in 13-20% of the DLAs, can be used to conclude that DLAs at z>1.9 could contribute as much as 50% star formation rate density seen in Lyman break galaxies (LBGs). (Abridged)