Name	E_mail_Address	Scientific_Session	Contribution_type	Title	Authors_affiliations	Abstract	
Fellhauer / Michael / Alois Dominik	madf@ast.cam.ac.uk	EAS Symp.6:Dynamics of Galaxies and Galactic Nuclei.	invited	The origin of the bifurcation of the Sagittarius stream or why the MW halo is spherical	M. Fellhauer, N.W. Evans (IoA, Cambridge)	The latest Sloan Digital Sky Survey data tracing the tidal stream from
the Sagittarius dwarf spheroidal (dSph) reveals a bifurcation in the
distribution of debris.  The bifurcation is caused by the projection
of the old trailing and young leading tidal arms of the Sagittarius
dSph.  The existence and location of this bifurcation places the
strongest constraints to date on the shape of the halo. Using
numerical simulations, we find that the halo of our Galaxy has to be
close to spherical. This result is not sensitive to variations in the
proper motion of Sagittarius (within the observationally permitted
range) and is also robust to changes in the details of the Milky Way
potential.