  Our boundary-value approach to quantum processes in the gravitational
collapse to a black hole leads to quantum amplitudes (not just probabilities)
for transitions between data posed on initial and final hypersurfaces
$\Sigma_{I,F}$, separated by a Lorentzian proper-time interval $T$, measured at
spatial infinity. Following Feynman's $+i\epsilon$ approach, we rotate: $T\to
{\mid}T{\mid} \exp(-i\theta)$, for $0<\theta\leq\pi/2$. The {\it classical}
complexified boundary-value problem is expected to be well-posed for
$0<\theta\leq\pi/2$, with classical action $S_{\rm class}$. For a locally
supersymmetric Lagrangian, containing supergravity, possibly coupled to
supermatter, the resulting quantum amplitude will be proportional to
$\exp(iS_{\rm class})$, apart from possible loop corrections which are
negligible for boundary data with frequencies below the Planck scale. The
Lorentzian quantum amplitude is recovered by taking the limit as $\theta\to
0_+$ of this amplitude. In the present paper, a connection is made between this
boundary value approach and the original approach to quantum evaporation in
gravitational collapse to a black hole, {\it via} Bogoliubov coefficients. This
connection is developed through consideration of the radial equation obeyed by
the (adiabatic) non-spherical classical perturbations. When one studies the
resulting final probability distribution, based on our quantum amplitudes
above, one finds that this distribution can also be interpreted in terms of the
Wigner quasi-probability distribution for harmonic oscillators.
