This article has an erratum: [erratum]
Volume 380, Number 1, December II 2001
|Page(s)||117 - 122|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 December 2001|
Unusual metal abundances in a pair of damped Lyman alpha systems at *
European Southern Observatory, Casilla 19001, Santiago 19, Chile e-mail: email@example.com
2 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile e-mail: firstname.lastname@example.org
Corresponding author: S. Ellison, email@example.com
Accepted: 9 October 2001
We present high resolution spectroscopic observations of two neighbouring damped Lyman α systems (DLAs) along the same line of sight towards B2314-409. Due to their separation ( km s-1) and the high spectral resolution of the data, it is possible to fit not only the weak metal transitions, but also the separate H I absorption profiles. This has permitted, for the first time, a detailed study of metal abundances in two neighbouring galaxy-scale absorbers. The two DLAs have zabs = 1.8573 and 1.8745 and have column densities N(H I) = and respectively. We have determined abundances for a range of chemical elements, and find that both absorbers towards B2314-409 have low α/Fe-peak abundances compared with other known DLAs. This indicates that not only has the recent star formation history of these absorbers been relatively passive, but that the group environment, or some other external factor, may have influenced this.
Key words: quasars: general / quasars: absorption lines / quasars: individual: B2314-409 / galaxies: evolution / galaxies: clusters: general
© ESO, 2001
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.