Gamma ray and neutrino flux from the annihilation of neutralino dark matter at the Galactic halo region in the mAMSB model

Abstract

We consider the lightest supersymmetric particle (LSP), neutralino in minimal anomaly mediated supersymmetry breaking model (mAMSB) to be a possible candidate for weakly interacting massive particles (WIMP) or cold dark matter and investigate its direct and indirect detections. The theoretically allowed supersymmetric parametric space for such a model along with the recent bounds from LHC is constrained by the WMAP results for relic densities. The spin independent and spin dependent scattering cross sections for dark matter off nucleon are thus constrained from the WMAP results. They are found to be within the allowed regions of different ongoing direct detection experiments. The annihilation of such dark matter candidates at the galactic centre produce different standard model particles such as gamma rays, neutrinos etc. In this work, we calculate the possible fluxes of these γ-rays and neutrinos coming from the direction of the galactic centre (and its neighbourhood) at terrestrial or satellite borne detectors. The calcutated γ-ray flux is compared with the observational results of HESS experiment. The neutrino flux of different flavours from the galactic centre and at different locations away from the galactic centre produced by WIMP annihilation in this model are also obtained for four types of galactic dark matter halo profiles. The detection prospects of such ν µ coming from the direction of the galactic centre at the ANTARES under sea detector are discussed in terms of muon signal yield from these muon neutrinos. Both the gamma and neutrino signals are estimated for four different dark matter halo profiles.

A possible explanation of low energy γ-ray excess from galactic centre and Fermi bubble by a Dark Matter model with two real scalars

“…The XENON 100 benchmark point 4A is used for figure 12, where we see that for DM masses ∼ 55 GeV and for all DM profiles other than the cuspy Moore profile, the DM annihilation contribution is rather small compared to contributions from point sources and galactic ridge. NFW profile works better for XENON 100 benchmark point 4B, used for figure 13 5.1). SS-annihilation is calculated for M S = 8.6 GeV and δ 2 = 0.45 and is denoted by the dotted violet line.…”

“…Many such extensions have been suggested in the literature in the framework of supersymmetry, extra dimensions, axion etc. Models such as Kaluza Klein [10,11], inert triplet [12] or supersymmetry breaking models like mAMSB [13] predict very massive DM whereas models like SMSSM [14], axion [15] predict DM of lower mass. Phenomenology of simpler extensions of SM like fermionic DM model [16] or inert doublet model [17] has been elaborately studied.…”

3.5 keV X-ray line signal from decay of right-handed neutrino due to transition magnetic moment

“…The feature of monochromatic line from such decay or annihilation of DM is particularly significant in predicting the nature of DM particles. A huge variety of DM models in the framework of WIMP scenario with masses of DM spanning from keV to TeVs has been addressed in several literatures and their direct and indirect detection prospects have been widely studied [5][6][7][8][9][10][11][12][13][14][15][16][17][18].…”