A quantum Schwarzschild black hole is described, at the mini super spacetime level, by a nonsingular wave packet composed of plane wave eigenstates of the momentum Dirac-conjugate to the mass operator. The entropy of the mass spectrum acquires then independent contributions from the average mass and the width. Hence, Bekenstein's area entropy is formulated using the mass 2 average, leaving the mass average to set the Hawking temperature. The width function peaks at the Planck scale for an elementary (zero entropy, zero free energy) micro black hole of finite rms size, and decreases Doppler-like towards the classical limit.

If general relativity is spontaneously induced, that is if the reciprocal Newton constant serves as a vacuum expectation value, the electrically charged black hole limit is governed by a Davidson-Gurwich phase transition which occurs precisely at the would-have-been outer horizon. The transition profile which connects the exterior Reissner-Nordstrom solution with the novel interior is analytically derived. The inner core is characterized by a vanishing spatial volume and constant surface gravity, and in some respects, resembles a maximally stretched horizon. The Komar mass residing inside any concentric interior sphere is proportional to the surface area of that sphere, and consequently, is non-negative definite and furthermore nonsingular at the origin. The Kruskal structure is recovered, admitting the exact Hawking imaginary time periodicity, but unconventionally, with the conic defect defused at the origin. The corresponding holographic entropy packing locally saturates the 't Hooft-Susskind-Bousso holographic bound, thus making the core Nature's ultimate information storage.

Applying Dirac's procedure to r-dependent constrained systems, we derive a reduced total Hamiltonian, resembling an upside down harmonic oscillator, which generates the Schwarzschild solution in the mini super-spacetime. Associated with the now r-dependent Schrodinger equation is a tower of localized Guth-Pi-Barton wave packets, orthonormal and non-singular, admitting equally spaced average-'energy' levels. Our approach is characterized by a universal quantum mechanical uncertainty structure which enters the game already at the flat spacetime level, and accompanies the massive Schwarzschild sector for any arbitrary mean mass. The average black hole horizon surface area is linearly quantized.

Mini superspace cosmology treats the scale factor a(t), the lapse function n(t), and an optional dilation field φ(t) as canonical variables. While pre-fixing n(t) means losing the Hamiltonian constraint, pre-fixing a(t) is serendipitously harmless at this level. This suggests an alternative to the Hartle-Hawking approach, where the pre-fixed a(t) and its derivatives are treated as explicit functions of time, leaving n(t) and a now mandatory φ(t) to serve as canonical variables. The naive gauge pre-fix a(t) = const is clearly forbidden, causing evolution to freeze altogether, so pre-fixing the scale factor, say a(t) = t, necessarily introduces explicit time dependence into the Lagrangian. Invoking Dirac's prescription for dealing with constraints, we construct the corresponding mini superspace time dependent total Hamiltonian, and calculate the Dirac brackets, characterized by {n, φ} D = 0, which are promoted to commutation relations in the quantum theory.

Pre-gauging the cosmological scale factor a(t) does not introduce unphysical degrees of freedom into the exact FLRW classical solution. It seems to lead, however, to a non-dynamical mini superspace. The missing ingredient, a generalized momentum enjoying canonical Dirac (rather than Poisson) brackets with the lapse function n(t), calls for measure scaling which can be realized by means of a scalar field. The latter is essential for establishing a geometrical connection with the 5-dimensional Kaluza-Klein Schwarzschild-deSitter black hole. Contrary to the Hartle-Hawking approach, (i) The t-independent wave function ψ(a) is traded for an explicit t-dependent ψ(n, t), (ii) The classical FLRW configuration does play a major role in the structure of the 'most classical' cosmological wave packet, and (iii) The non-singular Euclid/Lorentz crossovers get quantum mechanically smeared.