A&A 384, 140-144 (2002)
DOI: 10.1051/0004-6361:20020016

Using Cepheids to determine the galactic abundance gradient

II. Towards the galactic center

S. M. Andrievsky^{1, 2}, D. Bersier³, V. V. Kovtyukh^{2, 4}, R. E. Luck⁵, W. J. Maciel¹, J. R. D. Lépine¹ and Yu. V. Beletsky<sup>2, 4

1</sup>  Instituto Astronômico e Geofísico, Universidade de São Paulo, Av. Miguel Stefano, 4200 São Paulo SP, Brazil
²  Department of Astronomy, Odessa State University, Shevchenko Park, 65014 Odessa, Ukraine
    e-mail: scan@deneb.odessa.ua; val@deneb.odessa.ua
³  Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 16, Cambridge, MA 02138, USA
    e-mail: dbersier@cfa.harvard.edu
⁴  Odessa Astronomical Observatory and Isaac Newton Institute of Chile, Odessa Branch, Ukraine
⁵  Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106-7215, USA
    e-mail: luck@fafnir.astr.cwru.edu

(Received 23 November 2001 / Accepted 19 December 2001 )

Abstract
Based on spectra obtained at the Anglo-Australian Observatory, we present a discussion of the metallicity of the galactic disc derived using Cepheids at galactocentric distances of 4-6 kpc. Our new results together with previous gradient determination (Paper I) show that the overall abundance distribution within the galactocentric distances 4-11 kpc cannot be represented by a single gradient value. The distribution is more likely bimodal: it is flatter in the solar neighbourhood with a small gradient, and steepens towards the galactic center. The steepening begins at a distance of about 6.6 kpc.

Key words: stars: abundances -- stars: Cepheids -- Galaxy: abundances -- Galaxy: evolution

Offprint request: S. M. Andrievsky, sergei@andromeda.iagusp.usp.br

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