C, N, O Abundances in the Most Metal-Poor Damped Lyman alpha Systems

Details C, N, O Abundances in the Most Metal-Poor Damped Lyman alpha Systems C, N, O Abundances in the Most Metal-Poor Damped Lyman alpha Systems

2007-12-11

arxiv.org/abs/0712.1829v2

Astronomy and Astrophysics

Astrophysics

17 pages, 9 Figures, Accepted for publication in Monthly Notices of the Royal Astronomical Society

Scientific paper

10.1111/j.1365-2966.2008.12951.x

This study focuses on some of the most metal-poor damped Lyman alpha absorbers known in the spectra of high redshift QSOs, using new and archival observations obtained with UV-sensitive echelle spectrographs on the Keck and VLT telescopes. The weakness and simple velocity structure of the absorption lines in these systems allows us to measure the abundances of several elements, and in particular those of C, N, and O, a group that is difficult to study in DLAs of more typical metallicities. We find that when the oxygen abundance is less than about 1/100 of solar, the C/O ratio in high redshift DLAs and sub-DLAs matches that of halo stars of similar metallicity and shows higher values than expected from galactic chemical evolution models based on conventional stellar yields. Furthermore, there are indications that at these low metallicities the N/O ratio may also be above simple expectations and may exhibit a minimum value, as proposed by Centurion and her collaborators in 2003. Both results can be interpreted as evidence for enhanced production of C and N by massive stars in the first few episodes of star formation, in our Galaxy and in the distant proto-galaxies seen as QSO absorbers. The higher stellar yields implied may have an origin in stellar rotation which promotes mixing in the stars' interiors, as considered in some recent model calculations. We briefly discuss the relevance of these results to current ideas on the origin of metals in the intergalactic medium and the universality of the stellar initial mass function.

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