  Quantum fluctuations created during inflation can account for the observed
matter distribution in the linear regime if the universe has two components of
dark matter, one which is cold and collisionless, and the other which is hot
and free streams on small scales. However, this free streaming property of the
hot component prevents early structure formation, and since objects, such as
damped Lyman-$\alpha$ systems, have been observed at high redshift, it is
necessary to produce more power on small scales. Here, we show that the
situation can be improved substantially in models where cosmic strings are
formed at the end of inflation, and in which both inflation and strings
participate in the generation of structure.
