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Mass Modelling of dwarf Spheroidal Galaxies

Published online by Cambridge University Press:  01 June 2007

Jarosław Klimentowski ,
Ewa L. Łokas ,
Stelios Kazantzidis ,
Francisco Prada ,
Lucio Mayer  and
Gary A. Mamon
Jarosław Klimentowski
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
Ewa L. Łokas
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
Stelios Kazantzidis
Affiliation:
Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, P.O. Box 20450, M/S 29, Stanford, CA 94309, USA
Francisco Prada
Affiliation:
Instituto de Astrofísica de Andalucia, Apartado Correos 3005, E-18080 Granada, Spain
Lucio Mayer
Affiliation:
Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland Institute of Astronomy, Department of Physics, ETH Zürich, Wolfgang-Pauli Strasse, CH-8093 Zürich, Switzerland
Gary A. Mamon
Affiliation:
Institut d'Astrophysique de Paris(UMR 7095: CNRS and Université Pierre & Marie Curie), 98 bis Bd Arago, F-75014 Paris, France GEPI (UMR 8111: CNRS and Université Denis Diderot), Observatoire de Paris, F-92195 Meudon, France
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Abstract

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We study the origin and properties of unbound stars in the kinematic samples of dwarf spheroidal galaxies. For this purpose we have run a high resolution N-body simulation of a two-component dwarf galaxy orbiting in a Milky Way potential. We create mock kinematic data sets by observing the dwarf in different directions. When the dwarf is observed along the tidal tails the kinematic samples are strongly contaminated by unbound stars from the tails. However, most of the unbound stars can be removed by the method of interloper rejection proposed by den Hartog & Katgert. We model the velocity dispersion profiles of the cleaned-up kinematic samples using solutions of the Jeans equation. We show that even for such a strongly stripped dwarf the Jeans analysis, when applied to cleaned samples, allows us to reproduce the mass and mass-to-light ratio of the dwarf with accuracy typically better than 25%.

Keywords

galaxies: dwarfgalaxies: Local Groupgalaxies: kinematics and dynamicsgalaxies: fundamental parameterscosmology: dark matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 321 - 325
Copyright
Copyright © International Astronomical Union 2008

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