Metallicities and Abundance Ratios from Quasar Broad Emission Lines

Details Metallicities and Abundance Ratios from Quasar Broad Emission Lines Metallicities and Abundance Ratios from Quasar Broad Emission Lines

2001-09-02

arxiv.org/abs/astro-ph/0109006v2

Astronomy and Astrophysics

Astrophysics

15 pages, 5 figures in 6 files, in press with ApJ. This version fixes some minor glitches and includes previously omitted refe

Scientific paper

10.1086/324289

The broad emission lines (BELs) of quasars and active galactic nuclei (AGNs) are important diagnostics of the relative abundances and overall metallicity in the gas. Here we present new theoretical predictions for several UV BELs. We focus specifically on the relative nitrogen abundance as a metallicity indicator, based on the expected secondary enrichment of nitrogen at metallicities Z > 0.2 Z_o. Among the lines we consider, N III] 1750/O III] 1664, N V 1240/(C IV 1549 + O VI 1034) and N V/He II 1640 are the most robust diagnostics. We argue, in particular, that the average N V BEL is not dominated by scattered Ly-alpha photons from a broad absorption line wind. We then compare our calculated line ratios with observations from the literature. The results support earlier claims that the gas-phase metallicities near quasars are typically near or several times above the solar value. We conclude that quasar activity is preceded by, or coeval with, an episode of rapid and extensive star formation in the surrounding galactic (or proto-galactic) nuclei. Chemical evolution models of these environments suggest that, to reach Z > Z_o in well-mixed interstellar gas, the star formation must have begun > 10^8 yr before the observed quasar activity.

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