  Research in cosmology traditionally divided into two separate lines. On the
one hand was the search for initial conditions: the cosmological parameters H,
Omega, Omega_b, and Lambda, and the power spectrum P(k). On the other hand was
the study of the formation and evolution of structures, from globular-cluster
sized objects to large-scale structures. These lines of investigation are now
becoming increasingly intertwined, and this tendency manifested itself in this
conference. Following is my personal perspective on where we stand today. I
also discuss some technological developments that I think will affect the
field. My concluding remarks are very informal. They are not a review paper,
and I omit references altogether rather than give a partial list.
