Abstract: The standard cosmological model, though works very well to explain the available cosmological data, is not free of problems. One of its major drawbacks is the presence of the initial cosmological singularity. The singularity is pointing out the incompleteness of the underlying theory, in this case general relativity. A possible approach to avoid the singularity is through a classical cosmological bounce from a previous contracting phase. During the contraction, the density and temperature of the cosmic fluid increases in such a way that all structure is expected to be erased. It is not clear, however, whether black holes formed before the bounce would survive to it. In this talk, I will address this problem. In particular, I will show that a black hole described by the Generalized McVittie metric persists during the contraction, bounce and expansion of the universe. This result implies that there is a class of bouncing models that admit black holes at all cosmological epochs. I will also discuss some implications of these results, and the role these surviving black holes might play in the subsequent expanding phase of the universe.