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In this work we have investigated the synergy between Stage-IV galaxy surveys and future GW observatories for constraining the underlying cosmological model of the Universe, focussing on photometric galaxy clustering, cosmic shear and GW magnification as cosmological probes. We have implemented a Fisher matrix approach for the evaluation of the full 62pt statistics composed by the angular power spectra of the single probes together with their combination. For our analysis, we have in particular considered dynamical dark energy and massive neutrino scenarios. We have found that the improvement to galaxy survey performance is below 1\%, in the case ^ GW ₌₀ₗ=100 and a luminosity distance error of ₃₋/dL=10\%. However, when extending the analysis to ^ GW ₌₀ₗ=1000, we find that the GW magnification improves the galaxy survey performance on all the cosmological parameters, reducing their errors by 3\%-5\%, when ₃₋/dL=10\%, and by 10\%-18\% when ₃₋/dL=1\%, especially for M_, w₀ and wₐ. However, here our analysis is unavoidably optimistic: a much more detailed and realistic approach will be needed, especially by including systematic effects. But we can conclude that, in the case of future gravitational wave observatories the inclusion of the gravitational wave magnification can improve Stage-IV galaxy surveys performance on constraining the underlying cosmological model of the Universe.
Beltrame et al. (Wed,) studied this question.