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The galactic binary GW noisewill be modulated by the LISA orbital motion,
whereas the extragalactic one will not. If the latter is comparable with
galactic values at some galactic latitudes, it can impede detection by LISA
of some interesting relic cosmological GW backgrounds,
and specific statistical features of the relic GW should be used to separate
them against the noise from astrophysical sources.

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The galactic binary GW noisewill be modulated by the LISA orbital motion,
whereas the extragalactic one will not.
If the latter is comparable with
galactic values at some galactic latitudes, it can impede detection by LISA
of some interesting relic cosmological GW backgrounds,
and specific statistical features of the relic GW should be used to separate
them against the noise from astrophysical sources.

Just crossing out text out, X out.

The galactic binary GW noisewill be modulated by the LISA orbital motion,
whereas the extragalactic one will not.
If the latter is comparable with
galactic values at some galactic latitudes, it can impede detection by LISA
of some interesting relic cosmological GW backgrounds,
and specific statistical features of the relic GW should be used to separate
them against the noise from astrophysical sources.

\end{document}