Metallicity Distributions of Elliptical Galaxies and Globular Cluster Systems |
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| Authors: | Nobuo Arimoto Chiaki Kobayashi |
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| Institution: | (1) Institute of Astronomy, School of Science, University of Tokyo, 2-21-1, Osawa, Mitaka, Tokyo 181, Japan;(2) Department of Astronomy, School of Science, University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo 113, Japan |
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| Abstract: | Gradients of absorption line indices are studied and mean stellar metallicities are estimated for 46 elliptical galaxies.
The mean stellar metallicities range from 〈 Fe/H] 〉 ≃ =0.8 to +0.2 and ellipticals with smaller central velocity dispersions
tend to have lower 〈 Fe/H] 〉 thus the mass-metallicity relation holds not only for the galaxy center but also for the whole
part of the galaxy. There is an evidence that the magnesium is enhanced systematically in all ellipticals by 0.2 dex with
respect to the iron. Giant elliptical galaxies show lack of metal-poor stars (the G-dwarf problem). Metal-poor globular clusters
of ellipticals formed well in advance of the formation of metal-rich ones which formed simultaneously with the bulk of stars
of mother galaxies under the influence of galaxy chemical enrichment. The bimodal Fe/H] distribution of globular clusters
does not necessarily mean that elliptical galaxies formed by the mergers of disc galaxies.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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