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Secondary infall model and dark matter scaling relations in intermediate-redshift early-type galaxies

Cardone, V. F. ; Del Popolo, A. ; Tortora, C. ; Napolitano, N. R.

In: Monthly Notices of the Royal Astronomical Society, 2011, vol. 416, no. 3, p. 1822-1835

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    Titre
    • Secondary infall model and dark matter scaling relations in intermediate-redshift early-type galaxies
    Auteur
    • Cardone, V. F.. I.N.A.F. - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Roma, Italy
    • Del Popolo, A.. Dipartimento di Fisica e Astronomia, Università di Catania, Viale Andrea Doria 6, 95125 Catania, Italy
    • Tortora, C.. Universität Zürich, Institut für Theoretische Physik, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    • Napolitano, N. R.. INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, Italy
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2011, vol. 416, no. 3, p. 1822-1835. Blackwell Publishing Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:299399
    Summary
    Scaling relations among dark matter (DM) and stellar quantities are a valuable tool to constrain formation scenarios and the evolution of galactic structures. However, most of the DM properties are actually not directly measured, but derived through model-dependent mass-mapping procedures. It is therefore crucial to adopt theoretically and observationally well founded models. We use here an updated version of the secondary infall model (SIM) to predict the halo density profile, taking into account the effects of angular momentum, dissipative friction and baryons collapse. The resulting family of halo profiles depends only on one parameter, the virial mass, and nicely fits the projected mass and aperture velocity dispersion of a sample of intermediate redshift lens galaxies. We derive DM-related quantities (namely the column density and the Newtonian acceleration) and investigate their correlations with stellar mass, luminosity, effective radius and virial mass