Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ap%26ss.276..767b&link_type=abstract
Astrophysics and Space Science, v. 276, Issue 2/4, p. 767-774 (2001).
Astronomy and Astrophysics
Astrophysics
4
Scientific paper
We investigate numerically the chemodynamical evolution of major disc-disc galaxy mergers in order to explore the origin of the mass-dependent chemical, photometric and spectroscopic properties observed in elliptical galaxies. We investigate especially the dependence of the fundamental properties on merger progenitor disc mass (M_d). Three main results are obtained in this study: - More massive (luminous) ellipticals formed by galaxy mergers between more massive spirals have higher metallicity (Z) and thus show redder colours; the typical metallicity ranges from ~ 1.0 solar abundance (Z~ 0.02) for ellipticals formed by mergers with M_d = 10^10M_solar to ~ 2.0 solar (Z~ 0.04) for those with M_d = 10^12 M_solar. - Both the Mg_2 line index in the central part of ellipticals (R <= 0.1 R_e) and the radial gradient of Mg_2 (δ Mg_2 / δ log R) are more likely to be larger for massive ellipticals. δ Mg_2 / δ log R correlates reasonably well with the central Mg_2 in ellipticals. For most of the present merger models, ellipticals show a positive radial gradient of the H_β line index. - Both M/L_B and M/L_K (where M, L_B, and L_K are the total stellar mass of galaxy mergers, the B-band and the K-band luminosities, respectively) depend on galactic mass in such a way that more massive ellipticals have larger M/L_B and smaller M/L_K.
Bekki Kenji
Shioya Yasuhiro
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