  A nearly black, gravitationally intense star of semi-transparent, spherical,
massive shell containing a few pointlike light sources inside would be
perceived not like a three-dimensional ball for a localized observer outside
the shell in terms of the affine or binocular distance. As the radius of the
spherical shell approaches the Schwarzschild radius, the perceived distance
between the front and rear surfaces of the shell would go to zero, while the
images of most of the interior emitters would squeeze around the shell surfaces
in terms of the affine or binocular distance. So, the Schwarzschild black hole
formed from the star would be thought of as a two-dimensional membrane for the
observers who can only measure the binocular distance and/or affine distance.
However, the depth information of a point source inside the nearly black star
can still be resolved in terms of the radar or luminosity distance, which needs
the knowledge about the radar signals or standard candles sent in earlier by
the observer outside the star. This suggests that at late times of
gravitational collapse the area law of the entropy would dominate over the
volume law for outside observers due to the loss of the knowledge about the
ingoing probes earlier.
