  We review the properties of Galactic binaries containing two compact objects,
as derived by means of population synthesis. Using this information we
calculate the gravitational wave signal of these binaries. At frequencies below
f ~< 2 mHz the double white dwarf population forms an unresolved background for
the low-frequency gravitational wave detector LISA. Above this limit some few
thousand double white dwarfs and few tens of binaries containing neutron stars
will be resolved. Of the resolved double white dwarfs ~500 have a total mass
above the Chandrasekhar limit. About ~95 of these have a measurable frequency
change allowing a determination of their chirp mass. We discuss the properties
of the resolved systems.
