(Left:) Nominal configuration of a dSph galaxy with a luminous dwarf
galaxy following a "cored" King profile-like distribution (several versions
shown in red, green and pink) embedded inside a "cusped" NFW profile (the outer,
A comparison between the final total mass ( solid lines) and the stellar mass profiles
( dot-dashed lines) for N-body, smoothed particle hydrodynamical simulations of initially
rotationally supported, two-component (i.e., luminous matter embedded in an extended dark matter
halo) dwarf galaxies that become tidally stirred and stripped while orbiting in a MW-like
potential, by Mayer et al. (2001).
The models include a low surface brightness (LSB) dwarf with disk scale length 4.4 kpc
that eventually turns into a dSph,
a high surface brightness (HSB) dwarf with a 2 kpc disk scale length
that eventually turns into a dwarf elliptical, and a very faint dIrr, like the LG system GR8, with
disk scale length 76 pc and a very high central dark matter density, that evolves into an extremely
dark matter dominated dSph, like Ursa Minor and Draco. Note that only in the last case does
the dark matter still greatly ``cocoon" the baryonic matter, whereas, particularly in the LSB/dSph case,
the end state is essentially a mass-follows-light system.