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Stellar population gradients from cosmological simulations: dependence on mass and environment in local galaxies

Tortora, C. ; Romeo, A. D. ; Napolitano, N. R. ; Antonuccio-Delogu, V. ; Meza, A. ; Sommer-Larsen, J. ; Capaccioli, M.

In: Monthly Notices of the Royal Astronomical Society, 2011, vol. 411, no. 1, p. 627-634

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    Titre
    • Stellar population gradients from cosmological simulations: dependence on mass and environment in local galaxies
    Auteur
    • Tortora, C.. Institut für Theoretische Physik, Universität Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    • Romeo, A. D.. Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 220, Santiago, Chile
    • Napolitano, N. R.. INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, Italy
    • Antonuccio-Delogu, V.. INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78, I-95123 Catania, Italy
    • Meza, A.. Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 220, Santiago, Chile
    • Sommer-Larsen, J.. Excellence Cluster Universe, Technische Universität München, Boltzmannstr. 2, D-85748 Garching bei München, Germany
    • Capaccioli, M.. Dipartimento di Scienze Fisiche, Università di Napoli Federico II, Compl. Univ. Monte S. Angelo, 80126 Napoli, Italy
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2011, vol. 411, no. 1, p. 627-634. Blackwell Publishing Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:295837
    Summary
    The age and metallicity gradients for a sample of group and cluster galaxies from N-body+hydrodynamical simulation are analysed in terms of galaxy stellar mass. Dwarf galaxies show null age gradient with a tail of high and positive values for systems in groups and cluster outskirts. Massive systems have generally zero-age gradients which turn to positive for the most massive ones. Metallicity gradients are distributed around zero in dwarf galaxies and become more negative with mass; massive galaxies have steeper negative metallicity gradients, but the trend flattens with mass. In particular, fossil groups are characterized by a tighter distribution of both age and metallicity gradients. We find a good agreement with both local observations and independent simulations. Interestingly, our results suggest that environment differently affects the gradients at low and high masses. The results are also discussed in terms of the central age and metallicity, as well as the total colour, specific star formation and velocity dispersion