N-body simulations of shell galaxies: two-component density models of cannibalized dwarfs

Abstract:
Insight into the process of creation of shell galaxies, which are thought to be by-products of minor mergers, can contribute to 
probing mass distribution of the progenitor-type objects. In the simplest situation, a dwarf satellite approaching a giant 
elliptical galaxy on a radial orbit, one can take advantage of the specific symmetry while studying such a merger. As the 
satellite galaxy is being gradually cannibalized, stars released from its potential, the least bound first, begin to oscillate on 
the close to the radial orbits in the gravitational well of the host galaxy and produce the moving stellar shell features at their 
turning points.
During its evolution, the debris system is sensitive to the mass distribution and to the related treatment of the gravitational
interaction. At the same time, similar setups can result into different shell structure, as the involving effects -- gradual decay 
of the satellite and dynamical friction -- have been changed.
In this poster we discuss the effect of the initial phase space structure of the satellite and of the host galaxy on the formation 
of the shell debris system in the TreePM simulations with the code GADGET-2. While creating initial conditions of merging 
galaxies, we use various self-consistent two-component density models (dark and luminous matter).