EDP Sciences
Free Access
Volume 397, Number 2, January II 2003
Page(s) 667 - 674
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20021530
Published online 17 December 2002

A&A 397, 667-674 (2003)
DOI: 10.1051/0004-6361:20021530

An estimate of the time variation of the O/H radial gradient from planetary nebulae

W. J. Maciel, R. D. D. Costa and M. M. M. Uchida

IAG/USP, 04301-904 São Paulo SP, Brazil
    e-mail: maciel@astro.iag.usp.br;roberto@astro.iag.usp.br;monica@astro.iag.usp.br
(Received 8 July 2002 / Accepted 18 October 2002 )

Radial abundance gradients are a common feature of spiral galaxies, and in the case of the Galaxy both the magnitude of the gradients and their variations are among the most important constraints of chemical evolution models. Planetary nebulae (PN) are particularly interesting objects to study the gradients and their variations. Owing to their bright emission spectra, they can be observed even at large galactocentric distances, and the derived abundances are relatively accurate, with uncertainties of about 0.1 to 0.2 dex, particularly for the elements that are not synthesized in their progenitor stars. On the other hand, as the offspring of intermediate mass stars, with main sequence masses in the interval of 1 to 8 solar masses, they are representative of objects with a reasonable age span. In this paper, we present an estimate of the time variation of the O/H radial gradient in a sample containing over 200 nebulae with accurate abundances. Our results are consistent with a flattening of the O/H gradient roughly from -0.11 dex/kpc to -0.06 dex/kpc during the last 9 Gyr, or from -0.08 dex/kpc to -0.06 dex/kpc during the last 5 Gyr.

Key words: Galaxy: abundances -- Galaxy: evolution -- planetary nebulae: general

Offprint request: W. J. Maciel, maciel@astro.iag.usp.br

© ESO 2003

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