Metal abundances and kinematics of quasar absorbers*
I. Absorption systems toward J2233–606
Division of Theoretical Astrophysics, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
2 Department of Theoretical Astrophysics, Ioffe Physico-Technical Institute, 194021 St. Petersburg, Russia
3 Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34131 Trieste, Italy
Corresponding author: S. A. Levshakov, email@example.com
Accepted: 18 December 2001
The metal line profiles of different ions observed in high column density systems [ N() cm-2] in quasar spectra can be used to constrain the ionization structure and kinematic characteristics of the absorbers. For these purposes, a modified Monte Carlo Inversion (MCI) procedure was applied to the study of three absorption systems in the spectrum of the HDF-South quasar J2233–606 obtained with the UVES spectrograph at the VLT/Kueyen telescope. The MCI does not confirm variations of metal abundances within separate systems which were discussed in the literature. Instead, we found that an assumption of a homogeneous metal content and a unique photoionizing background is sufficient to describe the observed complex metal profiles. It was also found that the linear size L and the line-of-sight velocity dispersion measured within the absorbers obey a scaling relation, namely, increases with increasing L, and that metal abundance is inversely proportional to the linear size of the system: the highest metallicity was measured in the system with the smallest L.
Key words: cosmology: observations / line: formation / line: profiles / galaxies: abundances / quasars: absorption lines / quasars: individual: J2233–606
Based on public data released from UVES Commissioning at the VLT Kueyen telescope (ESO, Paranal, Chile), the New Technology Telescope (ESO, La Silla, Chile) and the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities of Research in Astronomy, Inc. under NASA contract NAS 5-26555.
© ESO, 2002