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On the difference in formation history between bulges and ellipticals

Published online by Cambridge University Press:  07 August 2017

B. Rocca–Volmerange  and
O. K. Sil'chenko
B. Rocca–Volmerange
Affiliation:
1Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F—75014, Paris
O. K. Sil'chenko
Affiliation:
2Sternberg Astronomical Institute, University av. 13, 119899 Moscow

Abstract

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On the diagram (Fe5270, Mg5175) ellipticals and bulges of disk galaxies (from S0 to Sc) maintain a very different position: E's seem to be overabundant in Mg, bulges seem to have a solar ratio Mg/Fe, except several ones who are overabundant in Fe.

Type
Contributed Papers
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 431 - 432
Copyright
Copyright © Kluwer 1993 

References

1. Faber, S.M., Worthey, G., Gonzalez, J.J., 1991. In Stellar Populations of Galaxies, IAU Symposium 149, Eds. Barbuy, B. & Renzini, A. (Dordrecht: Kluwer), p.255.Google Scholar
2. Gilmore, G., & Wyse, R.F.G., 1991. Astrophys. J., 367, L55.Google Scholar
3. Guiderdoni, B., & Rocca–Volmerange, B., 1987. Astron. Astrophys., 186, 1.Google Scholar
4. Sil'chenko, O.K., & Shapovalova, A.I., 1989. Soobshch. Spets. Astrofiz. Obs., No.60, 44, or Preprint SAO RAS No.37.Google Scholar
5. Sil'chenko, O.K., 1990. Soobshch. Spets. Astrofiz. Obs., No.65, 75, or Preprint SAO RAS No.42.Google Scholar