Abstract
Supernovae can produce vast fluxes of new particles with masses on the MeV scale, a mass scale of interest for models of light dark matter. When these new particles become diffusively trapped within the supernova, the escaping flux will emerge semirelativistic with an order-one spread in velocities. As a result, overlapping emissions from Galactic supernovae will produce an overall flux of these particles at Earth that is approximately constant in time. However, this flux is highly anisotropic and is steeply peaked towards the Galactic center. This is in contrast with the cosmological abundance of a WIMP-like dark matter which, due to the rotation of the Galaxy, appears to come from the direction of the Cygnus constellation. In this paper, we demonstrate the need for a directional detector to efficiently discriminate between a signal from a cold cosmological abundance of GeV-scale WIMPs and a signal from a hot population of supernova-produced MeV-scale dark matter.
Highlights
Several astrophysical measurements indicate that the majority of the matter in the Universe is cold and dark [1]
Given that the goal of this paper is to evaluate the capability of dark matter (DM) detectors tailored for weakly interacting massive particles (WIMP) searches to discriminate between WIMPs and models such as the one discussed in the previous sections, we employ in this study an region of interest (ROI) for the Xe-based detector of 1⁄24.9; 40; 9 keVnr [40]
In order to estimate the improvement in signal discrimination using angular information, we compute the approximate number of events to discriminate a WIMP and SNDM spectrum for our various scenarios (Table I) in our fiducial experimental setups
Summary
Several astrophysical measurements (including those of the cosmic microwave background, cluster and galaxy rotations, gravitational lensing, and big bang nucleosynthesis) indicate that the majority of the matter in the Universe is cold and dark (i.e., nonluminous and nonabsorbing) [1]. Taken together, these observations suggest the existence of at least one quasistable dark matter (DM) particle that is not predicted by the Standard Model of particle physics. A stable, weakly-interacting particle at the GeV scale in thermal equilibrium with the early Universe would reproduce the observed relic dark matter density. Particles of this mass can appear in many theories, for example, as the lightest superpartner in supersymmetric models that conserve R-parity [2] or as the lightest Kaluza-Klein particle in universal extra dimensions models [3]
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