Colour-magnitude relations and spectral line strengths in the Coma cluster

Details Colour-magnitude relations and spectral line strengths in the Coma cluster Colour-magnitude relations and spectral line strengths in the Coma cluster

1999-07-06

arxiv.org/abs/astro-ph/9907072v1

Astronomy and Astrophysics

Astrophysics

9 pages, 5 figures. Accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.1999.02941.x

We use the $C_{2}4668$, $Fe4383$, $H\gamma_A$ and $H\delta_A$ spectral absorption line indices, together with U- and V-band photometry of 101 galaxies in the Coma cluster, to investigate how mean age and metal abundance correlate with galaxy luminosity. In particular, we use the line index measurements to address the origin of the colour-magnitude relation (CMR). We find that the CMR in Coma is driven primarily by a luminosity-metallicity correlation. We additionally show evidence for a relation between age and luminosity, in the direction predicted by the semi-analytic hierarchical clustering models of Kauffmann & Charlot, but this is only present in the $C_24668$ index models, and could be an effect of the lack of non solar abundance ratios in the Worthey models used. By comparing deviations from the CMR, with deviations in absorption index from analogous `index-magnitude' relations, we find that colour deviations bluewards of the mean relation are strongly correlated with the hydrogen Balmer line series absorption. We show that the properties of these blue galaxies are consistent with the presence of a young stellar population in the galaxies, rather than with a reduced metallicity.

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