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Morphological evolution of discs in clusters

Mastropietro, Chiara ; Moore, Ben ; Mayer, Lucio ; Debattista, Victor P. ; Piffaretti, Rocco ; Stadel, Joachim

In: Monthly Notices of the Royal Astronomical Society, 2005, vol. 364, no. 2, p. 607-619

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    Titel
    • Morphological evolution of discs in clusters
    Autor
    • Mastropietro, Chiara. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    • Moore, Ben. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    • Mayer, Lucio. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    • Debattista, Victor P.. Astronomy Department, University of Washington, Seattle, WA 98195-1580, USA
    • Piffaretti, Rocco. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    • Stadel, Joachim. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    Dokumententyp
    • Postprint
    Sprache
    • Englisch
    Veröffentlicht in
    • Monthly Notices of the Royal Astronomical Society, 2005, vol. 364, no. 2, p. 607-619. Blackwell Science Ltd
    Andere elektronische Ausgabe
    OAI-PMH-ID
    • oai:doc.rero.ch:292852
    Summary
    The recent discovery of hidden non-axisymmetric and disc-like structures in bright Virgo dwarf elliptical and lenticular galaxies (dE/dSph/dS0) indicates that they may have late-type progenitors. Using N-body simulations we follow the evolution of disc galaxies within a Λ cold dark matter (ΛCDM) cluster simulated with 107 particles, where the hierarchical growth and galaxy harassment are modelled self-consistently. Most of the galaxies undergo significant morphological transformation, even at the outskirts of the cluster, and move through the Hubble sequence from late-type discs to dwarf spheroidals. None of the discs is completely destroyed, therefore they cannot be the progenitors of ultracompact dwarf (UCD) galaxies. The time evolution of the simulated galaxies is compared with unsharp masked images obtained from Very Large Telescope (VLT) data and the projected kinematics of our models with the latest high-resolution spectroscopic studies from the Keck and Palomar telescopes