Black holes with sufficiently large initial charge and mass will Hawking-evaporate towards the extremal limit. The emission slows as the temperature approaches zero, but still reaches the point where a single Hawking quantum would make the object superextremal, removing the horizon. We take this semiclassical prediction at face value and ask: When the emission occurs, what is revealed? Using a model of thin-shell collapse with subsequent accretion/evaporation by a null flux of ingoing positive/negative energy (charged Vaidya spacetime glued to a flat interior), we find two possible outcomes: (i) For shells that are initially very tightly bound, a timelike singularity forms and later appears; or (ii) for unbound or modestly bound shells, the matter re-emerges as a null shell that expands to infinity. This expanding remnant has been bathed in the ingoing Hawking quanta during evaporation and presumably carries correlations with the outgoing quanta, offering the attractive possibility of studying information paradox issues in a setup where spacetime curvatures are globally small, so that quantum gravity is not required. Even for ordinary black holes that evaporate down to the Planck size, we propose a radical new scenario for the interior: rather than forming a singularity, the collapsing matter settles onto an *outgoing* null trajectory *inside* the horizon for the entirety of evaporation.