Dark inverse Compton scattering of cosmic-ray electrons and positrons on ultralight dark photon dark matter produces a sub-MHz radio background that, compared with IMP-6, RAE-2, and Parker Solar Probe data, constrains the kinetic mixing below about 2e-6 for masses below 2e-17 eV.
Search for anisotropies in cosmic-ray positrons detected by the PAMELA experiment
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abstract
The PAMELA detector was launched on board of the Russian Resurs-DK1 satellite on June 15, 2006. Data collected during the first four years have been used to search for large-scale anisotropies in the arrival directions of cosmic-ray positrons. The PAMELA experiment allows for a full sky investigation, with sensitivity to global anisotropies in any angular window of the celestial sphere. Data samples of positrons in the rigidity range 10 GV $\leq$ R $\leq$ 200 GV were analyzed. This article discusses the method and the results of the search for possible local sources through analysis of anisotropy in positron data compared to the proton background. The resulting distributions of arrival directions are found to be isotropic. Starting from the angular power spectrum, a dipole anisotropy upper limit \delta = 0.166 at 95% C.L. is determined. Additional search is carried out around the Sun. No evidence of an excess correlated with that direction was found.
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Sub-MHz Radio Background from Ultralight Dark Photon Dark Matter
Dark inverse Compton scattering of cosmic-ray electrons and positrons on ultralight dark photon dark matter produces a sub-MHz radio background that, compared with IMP-6, RAE-2, and Parker Solar Probe data, constrains the kinetic mixing below about 2e-6 for masses below 2e-17 eV.