  The well-known BTZ black hole solution of (2+1) Einstein's gravity, in the
presence of a cosmological constant, is treated both at the classical and
quantum level. Classically, the imposition of the two manifest local Killing
fields of the BTZ geometry at the level of the full action results in a
mini-superspace constraint action with the radial coordinate playing the role
of the independent dynamical variable. The Noether symmetries of this reduced
action are then shown to completely determine the classical solution space,
without any further need to solve the dynamical equations of motion. At a
quantum mechanical level, all the admissible sets of the quantum counterparts
of the generators of the above mentioned symmetries are utilized as
supplementary conditions acting on the wave-function. These additional
restrictions, in conjunction with the Wheeler-DeWitt equation, help to
determine (up to constants) the wave-function which is then treated
semiclassically, in the sense of Bohm. The ensuing space-times are, either
identical to the classical geometry, thus exhibiting a good correlation of the
corresponding quantization to the classical theory, or are less symmetric but
exhibit no Killing or event horizon and no curvature singularity, thus
indicating a softening of the classical conical singularity of the BTZ
geometry.
