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Abundance Gradient in the Disk of NGC 300

Published online by Cambridge University Press:  01 June 2008

Marija Vlajić ,
Joss Bland-Hawthorn  and
Ken C. Freeman
Marija Vlajić
Affiliation:
Astrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH, UK email: vlajic@astro.ox.ac.uk
Joss Bland-Hawthorn
Affiliation:
Institute of Astronomy, School of Physics, University of Sydney, Australia email: jbh@physics.usyd.edu.au
Ken C. Freeman
Affiliation:
Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Australian National University, Australia email: kcf@mso.anu.edu.au
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Abstract

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The structure of the outer parts of galactic disks and the nature of their stellar populations are fundamental to our understanding of the formation and evolution of spiral galaxies. Ages and metallicity distributions of stars in the outermost regions of spiral disks provide important clues on how and when the disks are assembled. In our earlier work we trace the extended stellar disk of NGC 300 out to a radius of at least 10 disk scale lengths, with no sign of truncation. We now revisit the outer disk of NGC 300 in order to derive the metallicity distribution of the faint stellar population in its outskirts. We find that predominantly old stellar population in the outer disk exhibits a negative abundance gradient – as predicted by the chemical evolution models – out to about 10 kpc, followed by the metallicity plateau in the outermost disk.

Keywords

galaxies: abundancesgalaxies: individual (NGC 300)galaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 97 - 102
Copyright
Copyright © International Astronomical Union 2009

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