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Dark Matter Constraints from the Sagittarius Dwarf and Tail System

Published online by Cambridge University Press:  26 May 2016

Steven R. Majewski ,
David R. Law ,
Kathryn V. Johnston ,
Michael F. Skrutskie  and
Martin D. Weinberg
Steven R. Majewski
Affiliation:
University of Virginia, Dept. of Astronomy, P.O. Box 3818, Charlottesville, VA 22903-0818, USA
David R. Law
Affiliation:
University of Virginia, Dept. of Astronomy, P.O. Box 3818, Charlottesville, VA 22903-0818, USA
Kathryn V. Johnston
Affiliation:
Wesleyan University, Dept. of Astronomy, Middletown, CT 06459-0123, USA
Michael F. Skrutskie
Affiliation:
University of Virginia, Dept. of Astronomy, P.O. Box 3818, Charlottesville, VA 22903-0818, USA
Martin D. Weinberg
Affiliation:
University of Massachusetts, Dept. of Physics & Astronomy, 517 Lederle GRC, Amherst, MA 01003 USA

Abstract

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2MASS has provided a three-dimensional map of the > 360°, wrapped tidal tails of the Sagittarius (Sgr) dwarf spheroidal galaxy, as traced by M giant stars. With the inclusion of radial velocity data for stars along these tails, strong constraints exist for dynamical models of the Milky Way-Sgr interaction. N-body simulations of Sgr disruption with model parameters spanning a range of initial conditions (e.g., Sgr mass and orbit, Galactic rotation curve, halo flattening) are used to find parameterizations that match almost every extant observational constraint of the Sgr system. We discuss the implications of the Sgr data and models for the orbit, mass and M/L of the Sgr bound core as well as the strength, flattening, and lumpiness of the Milky Way potential.

Type
Part 6: The Galaxy
Information
Symposium - International Astronomical Union , Volume 220: Dark Matter in Galaxies , 2004 , pp. 189 - 194
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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