Time variation of radial gradients in the Galactic disk: electron temperatures and abundances

Free access article

Issue		A&A Volume 463, Number 2, February IV 2007


Page(s)		L13 - L16
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20066916

A&A 463, L13-L16 (2007)
DOI: 10.1051/0004-6361:20066916

Letter

Time variation of radial gradients in the Galactic disk: electron temperatures and abundances

W. J. Maciel¹, C. Quireza², and R. D. D. Costa¹

¹ Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG/USP), Universidade de São Paulo, Rua do Matão 1226, 05508-900 São Paulo SP, Brazil
e-mail: [maciel;roberto]@astro.iag.usp.br
² Observatório Nacional, Rua General José Cristino 77, 20921-400 Rio de Janeiro RJ, Brazil
e-mail: quireza@on.br

(Received 11 December 2006 / Accepted 9 January 2007 )

Abstract
Aims.We investigate the electron temperature gradient in the galactic disk as measured by young HII regions on the basis of radio recombination lines and the corresponding gradient in planetary nebulae (PN) based on [OIII] electron temperatures. The main goal is to investigate the time evolution of the electron temperature gradient and of the radial abundance gradient, which is essentially a mirror image of the temperature gradient.
Methods.The recently derived electron temperature gradient from radio recombination lines in HII regions is compared with a new determination of the corresponding gradient from planetary nebulae for which the progenitor star ages have been determined.
Results.The newly derived electron temperature gradient for PN with progenitor stars with ages in the 4-5 Gyr range is much steeper than the corresponding gradient for HII regions. These electron temperature gradients are converted into O/H gradients in order to make comparisons with previous estimates of the flattening rate of the abundance gradient.
Conclusions.It is concluded that the O/H gradient has flattened out in the past 5 Gyr at a rate of about 0.0094 dex kpc^-1 Gyr^-1, in good agreement with our previous estimates.

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

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