  A new solution for the endpoint of gravitational collapse is proposed. By
extending the concept of Bose-Einstein condensation to gravitational systems, a
cold, compact object with an interior de Sitter condensate phase and an
exterior Schwarzschild geometry of arbitrary total mass M is constructed. These
are separated by a phase boundary with a small but finite thickness of fluid
with eq. of state p= +rho, replacing both the Schwarzschild and de Sitter
classical horizons. The new solution has no singularities, no event horizons,
and a global time. Its entropy is maximized under small fluctuations and is
given by the standard hydrodynamic entropy of the thin shell, instead of the
Bekenstein-Hawking entropy. Unlike black holes, a collapsed star of this kind
is thermodynamically stable and has no information paradox.
