Tidal stirring of satellites with shallow density profiles prevents them from being too big to fail

Understand

The "too big to fail" problem is revisited by studying the tidal evolution of populations of dwarf satellites with different density profiles.

• The high resolution cosmological $\rm \Lambda CDM$ "ErisMod" set of simulations is used.
• These simulations can model both the stellar and dark matter components of the satellites, and their evolution under the action of the tides of a MW-sized host halo at a force resolution better than 10 pc.
• The stronger tidal mass loss and re-shaping of the mass distribution induced in satellites with $\gamma=0.6$ dark matter density distributions, as those resulting from the effect of feedback in hydrodynamical simulations of dwarf galaxy formation, is sufficient to bring the circular velocity profiles in agreement with the kinematics of MW's dSphs.