ref [90] · 2606.24868 · notice #1837 · dispute
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cially, while the monopole (all-sky-average) of this chiral V-mode may be difficult to measure, the anisotropies of the stochastic GWB are shown to be a sensitive to it (see, for instance Belgacem and Kamionkowski (2020); Sato-Polito and Kamionkowski (2022); Cruz et al. (2024)). This effect can be leveraged to impose constraints on˜𝑔NL, thereby offering complementary constraint on the parameter over the scales probed by surveys of LSS Philcox (2022); Hou et al. (2023). Section 4 addresses the transition from the theoretical prediction of the GWB to its observational characterization, focusing on its anisotropic component. In the nano-Hertz frequency band, the GWB is primarily sourced by the cosmic population of inspiraling Supermassive Black Hole Binaries(SMBHBs)Sesanaetal.(2008);Casey-Clydeetal.
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cially, while the monopole (all-sky-average) of this chiral V-mode may be difficult to measure, the anisotropies of the stochastic GWB are shown to be a sensitive to it (see, for instance Belgacem and Kamionkowski (2020); Sato-Polito and Kamionkowski (2022); Cruz et al. (2024)). This effect can be leveraged to impose constraints on˜𝑔NL, thereby offering complementary constraint on the parameter over the scales probed by surveys of LSS Philcox (2022); Hou et al. (2023). Section 4 addresses the transition from the theoretical prediction of the GWB to its observational characterization, focusing on its anisotropic component. In the nano-Hertz frequency band, the GWB is primarily sourced by the cosmic population of inspiraling Supermassive Black Hole Binaries(SMBHBs)Sesanaetal.(2008);Casey-Clydeetal