EDP Sciences
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Volume 392, Number 2, September III 2002
Page(s) 491 - 499
Section Galactic structure and dynamics
DOI http://dx.doi.org/10.1051/0004-6361:20021035

A&A 392, 491-499 (2002)
DOI: 10.1051/0004-6361:20021035

Using Cepheids to determine the galactic abundance gradient

III. First results for the outer disc
S. M. Andrievsky1, 2, V. V. Kovtyukh1, 2, R. E. Luck3, J. R. D. Lépine4, W. J. Maciel4 and Yu. V. Beletsky1, 2

1  Department of Astronomy, Odessa State University, Shevchenko Park, 65014 Odessa, Ukraine
    e-mail: val@deneb.odessa.ua; adelante@ukr.net
2  Odessa Astronomical Observatory and Isaac Newton Institute of Chile, Odessa Branch, Ukraine
3  Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106-7215, USA
    e-mail: luck@fafnir.astr.cwru.edu
4  Instituto Astronômico e Geofísico, Universidade de São Paulo, Rua do Matão 1226, São Paulo SP, Brazil
    e-mail: jacques@astro.iag.usp.br; maciel@astro.iag.usp.br

(Received 12 April 2002 / Accepted 25 June 2002)

As a continuation of our previous work, which concerned the radial abundance distribution in the galactic disc over the distances 4-10 kpc this paper presents the first results on the metallicity in the outer disc ( $R_{\rm G} > 10$ kpc). Based on high-resolution spectra obtained for 19 distant Cepheids we sampled galactocentric distances from 10 to 12 kpc. Combined with the results of our previous work on the inner and middle parts of the galactic disc, the present data enable one to study the structure of the radial abundance distribution over a large baseline. In particular, we find indications of a discontinuity in the radial abundance distribution for iron as well as a number of the other elements. The discontinuity is seen at a galactocentric distance $R_{\rm G} = 10$ kpc. This finding supports the results reported earlier by Twarog et al. (1997).

Key words: stars: abundances -- stars: cepheids -- galaxy: abundances -- galaxy: evolution

Offprint request: S. M. Andrievsky, scan@deneb.odessa.ua

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