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Chemical evolution of bulges at high redshift

Published online by Cambridge University Press:  01 July 2007

Antonio Pipino ,
Francesca Matteucci  and
Annibale D'Ercole
Antonio Pipino
Affiliation:
Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, U.K. email: axp@astro.ox.ac.uk Dipartimento di Astronomia, Universita di Trieste, Via G.B. Tiepolo 11, 34100 Trieste, Italy
Francesca Matteucci
Affiliation:
Dipartimento di Astronomia, Universita di Trieste, Via G.B. Tiepolo 11, 34100 Trieste, Italy
Annibale D'Ercole
Affiliation:
INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy
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Abstract

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We present a new class of hydrodynamical models for the formation of bulges (either massive elliptical galaxies or classical bulges in spirals) in which we implement detailed prescriptions for the chemical evolution of H, He, O and Fe. Our results hint toward an outside-in formation in the context of the supernovae-driven wind scenario. The build-up of the chemical properties of the stellar populations inhabiting the galactic core is very fast. Therefore we predict a non significant evolution of both the mass-metallicity and the mass-[α/Fe] relations after the first 0.5 − 1 Gyr. In this framework we explain how the observed slopes, either positive or negative, in the radial gradient of the mean stellar [α/Fe], and their apparent lack of any correlation with all the other observables, can arise as a consequence of the interplay between star formation and metal-enhanced internal gas flows.

Keywords

galaxies: elliptical and lenticularcDgalaxies: abundancesGalaxy: bulge
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 19 - 22
Copyright
Copyright © International Astronomical Union 2008

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