Next: Gravitational Wave Background from Previous: Galactic Gravitational Wave Background
General shape of the GWB formed by extragalactic binaries was considered in earlier works (Lipunov et al., 1987a, Hills et al., 1990). Now we turn to the question about how the GWB changes if one makes observations with a GW detector with a specific angular resolution . It is intuitively clear that at frequencies above the critical ones for our Galaxy, one will detect rare bright jerks produced by coalescing white dwarfs (at a rate of 1 per 100 year) and NS (at a rate of 1 per - year) in our Galaxy, against a background of the extragalactic stochastic GW. In analogy with our Galaxy, critical frequencies must exist for the extragalactic background. Above them only merging NS will cross a given frequency interval at a rate of up to 100 per year if one observes all galaxies within 200 Mpc. Firstly we consider GWB from close individual galaxies, and then will discuss overall extragalactic GWB. The same questions as for the Milky Way galaxy are addressed.