Although one of the two namesakes of the $\Lambda$CDM cosmological model, the hypothesis of cold dark matter existence still chiefly relies on its gravitational effects, whilst both direct and indirect detection via non-gravitational signatures have not yet been achieved.
Weakly interacting massive particles (WIMP) are a candidate cold relic with a mass from 0.1 GeV to several TeV: they might then annihilate or decay in $\gamma$ photons and contribute to the unresolved gamma-ray background (UGRB) detected by experiments such as Fermi – LAT. Even if dominated by an isotropic shot-noise component, a degree of anisotropy was detected in the past already in the autocorrelation angular power spectrum.
The subsequently detected UGRB-galaxies angular power spectrum cross-correlation further enhances such anisotropy, showing a link between the UGRB and the large scale structure of the Universe (LSS), and allows a better understanding of its composition: some classes of astrophysical objects, like Active Galactic Nuclei, are the most likely sources, but dark matter contributions are not excluded; at low redshifts, the astrophysical contribution should even be subdominant compared to WIMP annihilation or decay signatures, as shown in previous works. Within this general framework, we present a weighting scheme of the galaxy tracer distribution which proved effective in enhancing the anisotropic contribution of other shot-noise-dominated LSS tracers, such as cosmic rays and gravitational waves, and assess its efficiency in terms of signal-to-noise ratio and constraining power on the WIMP mass and its annihilation or decay cross-sections.