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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 inter­
esting relic cosmological GW backgrounds, and specific statistical features of the
relic GW should be used to separate them against the noise from astrophysical
sources.
Figure 1: Caption of the figure
The galactic binary GW noisewill be
modulated by the LISA orbital motion,
whereas the extragalactic one will not.
If the latter is comparable with galac­
tic values at some galactic latitudes, it
can impede detection by LISA of some
interesting relic cosmological GW back­
grounds, and specific statistical features
of the relic GW should be used to sepa­
rate them against the noise from astro­
physical 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 inter­
esting relic cosmological GW backgrounds, and specific statistical features of the
relic GW should be used to separate them against the noise from astrophysical
sources.
1