The inner structure and kinematics of the Sagittarius dwarf galaxy as a product of tidal stirring

Understand

The tidal stirring model envisions the formation of dwarf spheroidal (dSph) galaxies in the Local Group via the tidal interaction of disky dwarf systems with a larger host galaxy like the Milky Way.

• These progenitor disks are embedded in extended dark halos and during the evolution both components suffer strong mass loss.
• In addition, the disks undergo the morphological transformation into spheroids and the transition from ordered to random motion of their stars.
• Using collisionless N-body simulations we construct a model for the nearby and highly elongated Sagittarius (Sgr) dSph galaxy within the framework of the tidal stirring scenario.