Abstract
Insights from UV absorption lines that arise from gas in our own galaxy help us to interpret the composition of very distant gas systems that are seen in QSO spectra. For instance, what we know about the depletions of free atoms as they condense onto dust grains nearby can be applied elsewhere, so that we can differentiate between low intrinsic heavy element abundances and the effects of such depletions. Experience from recent, very sensitive observations indicate that some elements created by the r- and s-process neutron capture nucleosynthesis may show absorption features in other systems at about the 1 mÅ level. The abundance of chlorine in neutral form is strongly enhanced by the presence of H2. Thus a detectable Cl I absorption at 1347 Å should persuade us to search for and study the Lyman and Werner bands of this important molecule. Finally, in the course of vigorous research by many investigators in the field of UV absorption line spectroscopy, we have learned some important lessons on methodology and how to lessen the impact of errors.
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Jenkins, E.B. (1995). Lessons Learned from UV Absorption Lines at z=0. In: Meylan, G. (eds) QSO Absorption Lines. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-49458-4_20
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DOI: https://doi.org/10.1007/978-3-540-49458-4_20
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