Physical conditions in QSO absorbers from fine-structure absorption lines

We calculate theoretical population ratios of the ground fine-structure levels of some atoms/ions which typically exhibit UV lines in the spectra of QSO absorbers redward the Ly-α forest: C, C, O, Si and Fe. The most reliable atomic data available is employed and a variety of excitation mechanisms considered: collisions with several particles in the medium, direct excitation by photons from the cosmic microwave background radiation (CMBR) and fluorescence induced by a UV field present. The theoretical population ratios are confronted with the corresponding column density ratios of C i and C ii lines observed in damped Ly-α (DLA) and Lyman Limit (LL) systems collected in the recent literature to infer their physical conditions. The volumetric density of neutral hydrogen in DLA systems is constrained to be lower than tens of cm (or a few cm in the best cases) and the UV radiation field intensity must be lower than two orders of magnitude the radiation field of the Galaxy (one order of magnitude in the best cases). Their characteristic sizes are higher than a few pc (tens of pc in the best cases) and lower limits for their total masses vary from 10 to 10 solar masses. For the only LL system in our sample, the electronic density is constrained to be ne < 0.15 cm . We suggest that the fine-structure lines may be used to discriminate between the current accepted picture of the UV extragalatic background as the source of ionization in these systems against a local origin for the ionizing radiation as supported by some authors. We also investigate the validity of the temperature-redshift relation of the CMBR predicted by the standard model and study the case for alternative models.