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Tidal streams in a MOND potential: constraints from Sagittarius

Read, J. I. ; Moore, Ben

In: Monthly Notices of the Royal Astronomical Society, 2005, vol. 361, no. 3, p. 971-976

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    Titre
    • Tidal streams in a MOND potential: constraints from Sagittarius
    Auteur
    • Read, J. I.. Institute of Astronomy, Cambridge University, Madingley Road, Cambridge CB3 OHA
    • Moore, Ben. Institute of Theoretical Physics, University of Zürich, Wintherurestrasse 190, 8057 Zurich, Switzerland
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2005, vol. 361, no. 3, p. 971-976. Blackwell Science Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:297768
    Summary
    We compare orbits in a thin axisymmetric disc potential in Modified Newtonian Dynamics (MOND) with those in a thin disc plus near-spherical dark matter halo predicted by a ΛCDM cosmology. Remarkably, the amount of orbital precession in MOND is nearly identical to that which occurs in a mildly oblate CDM Galactic halo (potential flattening q= 0.9), consistent with recent constraints from the Sagittarius stream. Since very flattened mass distributions in MOND produce rounder potentials than in standard Newtonian mechanics, we show that it will be very difficult to use the tidal debris from streams to distinguish between a MOND galaxy and a standard CDM galaxy with a mildly oblate halo. If a galaxy can be found with either a prolate halo or one that is more oblate than q∼ 0.9 this would rule out MOND as a viable theory. Improved data from the leading arm of the Sagittarius dwarf—which samples the Galactic potential at large radii—could rule out MOND if the orbital pole precession can be determined to an accuracy of the order of ±1°