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Issue A&A
Volume 448, Number 3, March IV 2006
Page(s) 955 - 970
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20053763

A&A 448, 955-970 (2006)
DOI: 10.1051/0004-6361:20053763

The chemical composition of metal-poor emission-line galaxies in the Data Release 3 of the Sloan Digital Sky Survey

Y. I. Izotov1, G. Stasinska2, G. Meynet3, N. G. Guseva1 and T. X. Thuan4

1  Main Astronomical Observatory, Ukrainian National Academy of Sciences, Zabolotnoho 27, Kyiv 03680, Ukraine
    e-mail: izotov@mao.kiev.ua
2  LUTH, Observatoire de Meudon, 92195 Meudon Cedex, France
3  Geneva Observatory, 1290 Sauverny, Switzerland
4  Astronomy Department, University of Virginia, Charlottesville, VA 22903, USA

(Received 5 July 2005 / Accepted 15 November 2005)

Abstract
We have re-evaluated empirical expressions for the abundance determination of N, O, Ne, S, Cl, Ar and Fe taking into account the latest atomic data and constructing an appropriate grid of photoionization models with state-of-the art model atmospheres. Using these expressions we have derived heavy element abundances in the ~310 emission-line galaxies from the Data Release 3 of the Sloan Digital Sky Survey (SDSS) with an observed H$\beta$ flux F(H$\beta$) > 10-14 erg s-1 cm-2 and for which the [O III] $\lambda$4363 emission line was detected at least at a 2$\sigma$ level, allowing abundance determination by direct methods. The oxygen abundance 12 + log O/H of the SDSS galaxies lies in the range from ~7.1 ($Z_\odot$/30) to ~8.5 (0.7 $Z_\odot$). The SDSS sample is merged with a sample of 109 blue compact dwarf (BCD) galaxies with high quality spectra, which contains extremely low-metallicity objects. We use the merged sample to study the abundance patterns of low-metallicity emission-line galaxies. We find that extremely metal-poor galaxies (12 + log O/H < 7.6, i.e. Z < $Z_\odot$/12) are rare in the SDSS sample. The $\alpha$ element-to-oxygen abundance ratios do not show any significant trends with oxygen abundance, in agreement with previous studies, except for a slight increase of Ne/O with increasing metallicity, which we interpret as due to a moderate depletion of O onto grains in the most metal-rich galaxies. The Fe/O abundance ratio is smaller than the solar value, by up to 1 dex at the high metallicity end. We also find that Fe/O increases with decreasing H$\beta$ equivalent width EW(H$\beta$). We interpret this as a sign of strong depletion onto dust grains, and gradual destruction of those grains on a time scale of a few Myr. All the galaxies are found to have log N/O > -1.6, implying that they have a different nature than the subsample of high-redshift damped Ly$\alpha$ systems with log N/O of ~-2.3 and that their ages are larger than 100-300 Myr. We confirm the apparent increase in N/O with decreasing EW(H$\beta$), already shown in previous studies, and explain it as the signature of gradual nitrogen ejection by massive stars from the most recent starburst.


Key words: galaxies: ISM -- galaxies: starburst -- galaxies: abundances

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© ESO 2006


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