Abstract
We review the properties of metal-rich absorption line systems derived from statistical studies of homogeneous samples. There is some evidence of evolution in the MgII line density with redshift but larger samples are needed to confirm this trend. The absorption systems can differ by their ionization level and by the strength of their lines. There is a strong correlation between the opacity to UV radiation of the absorbing clouds and their ionization level which implies that the neutral and singly ionized elements are present only in transition regions of large optical depth to UV ionizing photons. The heavy element abundances can be roughly estimated for systems with large HI column densities. They are a few tenths of the solar values. Even in the clouds with largest HI column densities there is no detection of dust. We present results of our search for the galaxies giving rise to MgII absorption line systems at redshift z<l. We compare properties of these galaxies with those derived from statistical studies of MgII absorption systems. From our high identification rate of the absorbing galaxies we infer strong constraints on their luminosity function at z~0.4. These galaxies have very large gaseous envelopes and show signs of strong stellar formation activity. They are usually field galaxies.
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Bergeron, J. (1988). Metal-Rich Absorption Line Systems. In: Kaiser, N., Lasenby, A.N. (eds) The Post-Recombination Universe. NATO ASI Series, vol 240. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3035-3_23
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DOI: https://doi.org/10.1007/978-94-009-3035-3_23
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