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Black holes are expected to evaporate through the process of Hawkingradiation. This process is expected to cause the uncertainty in a black hole'sposition to grow to $\sim M^2/M_{Pl}^3$ over the course of it's lifetime, evenas its momentum spreads only by $\sim M_{Pl}$. For the black holes that havebeen observed, which have $M\geq M_\odot$, this greatly exceeds the Hubblevolume. However, the decay of black holes and their quantum spreading, aredelayed in the Universe while the influx of energy into the black holes exceedstheir Hawking luminosity. We show that for these $M\geq M_\odot$ black holes,their decay outside galaxies and clusters is prevented far longer than it takesthe black holes to be dragged well beyond the Hubble horizon, where theireventual decay occurs away from the prying eyes of any observer who has nothitched a ride with them. Meanwhile, black holes in an observer's galaxy orcluster are themselves prevented from decaying long past the extinction of thelast stars, and at least until their galaxy/cluster is swept clean of darkmatter, in $\gg 10^{25}$y. Even then, if the black holes become unbound theyare dragged beyond the Hubble radius before undergoing significant decay; ifnot, they remain in bound orbits, spreading at most over a subvolume of thegalaxy/cluster, and long localized by scatterings to much smaller volumes.

How the Universe postpones the evaporation and curtails the quantum spreading of black holes