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The stochastic binary background produced by nearby galaxies from Tully's catalog at the frequency Hz is shown in Figure 49 in terms of average strain metric amplitude per square degree in a given direction (l,b) on the sky:
where the sum is calculated over all sources in the given square degree of the sky; we assumed .
The lines of constant on the sky (so-called isograwes) are plotted in Figure 50. As we expected (see Section 15.9), only the closest and most massive galaxies (such as SMC, LMC, M31, M82, M87) can be clearly discerned by a GW detector with angular resolution of 1 against the galactic binary GW stochastic background.
Figure: Stochastic GWB produced by binaries from Tully's catalog
against the GWB from our Galaxy at the frequency
Hz, in terms of mean strain metric amplitude per square degree in a given
direction (Lipunov et al., 1995a).
Figure 50: The ``isograwes'' from Figure 49
projected on to (l,b)-plane (Lipunov
et al., 1995a).