In the framework of indirect dark matter searches we investigate the flux of high energy gamma-ray photons produced by annihilation of dark matter in caustics within our Galaxy under the hypothesis that the bulk of dark matter is composed of the lightest supersymmetric particles. Unfortunately, the detection of the caustic annihilation signal with currently available instruments is rather challenging. Indeed, with realistic assumptions concerning particle physics and cosmology, the gamma-ray signal from caustics is below the detection threshold of both. Cerenkov telescopes and satellite-borne experiments. Nevertheless, we find that this signal is more prominent than that expected if annihilation only occurs in the smoothed Galactic halo, with the possible exception of a similar to 15 degrees circle around the Galactic centre if the mass density pro. le of our Galaxy exhibits a sharp cusp there. We show that the angular distribution of this gamma-ray flux changes significantly if DM annihilation preferentially occurs within virialized sub-haloes populating our Galaxy rather than in caustics.

gamma-ray flux from dark matter annihilation in galactic caustics

BRANCHINI, ENZO FRANCO
2005

Abstract

In the framework of indirect dark matter searches we investigate the flux of high energy gamma-ray photons produced by annihilation of dark matter in caustics within our Galaxy under the hypothesis that the bulk of dark matter is composed of the lightest supersymmetric particles. Unfortunately, the detection of the caustic annihilation signal with currently available instruments is rather challenging. Indeed, with realistic assumptions concerning particle physics and cosmology, the gamma-ray signal from caustics is below the detection threshold of both. Cerenkov telescopes and satellite-borne experiments. Nevertheless, we find that this signal is more prominent than that expected if annihilation only occurs in the smoothed Galactic halo, with the possible exception of a similar to 15 degrees circle around the Galactic centre if the mass density pro. le of our Galaxy exhibits a sharp cusp there. We show that the angular distribution of this gamma-ray flux changes significantly if DM annihilation preferentially occurs within virialized sub-haloes populating our Galaxy rather than in caustics.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11567/1072402
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