Astrophysical inputs on the SUSY dark matter annihilation detectability

Abstract

If dark matter (DM), which is considered to constitute most of the mass of galaxies, is made of supersymmetric (SUSY) particles, the centers of galaxies should emit gamma-rays produced by their self-annihilation. We present accurate estimates of continuum gamma-ray fluxes due to neutralino annihilation in the central regions of the Milky Way. We use detailed models of our Galaxy, which satisfy available observational data, and include some important physical processes, which were previously neglected. Our models predict that spatially extended annihilation signal should be detected at high confidence levels by incoming experiments assuming that neutralinos make up most of the DM in the Universe and that they annihilate according to current SUSY models.

Figures (2)

• Figure 1: Density and mass profiles for the Milky Way Galaxy. Symbols on right panel show observational constraints as taken from Klypin et al. Klypin02. The full and dashed curves labeled "Total" are total mass in NFW and Moore et al. models with adiabatic compression. DM mass in the NFW model is shown by the thick curve. In the central region most of the mass is in baryons. Left panel shows the density. The top full curve is the density of baryons. The dashed and full curves labeled "DM" are for the Moore et al. and NFW models with adiabatic compression. The long-dashed curve is the uncompressed NFW profile for comparison.
• Figure 2: Predicted continuum gamma flux as a function of distance $\Psi_0$ from the Galactic Center for Models A and B. The thick line shows the flux for the compressed NFW DM density profile of the Model A and the thin line for the compressed Moore et al. profile of the Model B. The flux profile for the uncompressed NFW profile is also shown for comparison (dotted line). The dashed line give the minimum detectable gamma flux F$_{\rm min}$ at $5\sigma$ level for exposure of 250 hours and E$_{\rm th}$=100 GeV for a typical IACT. The inserted pannel shows the YSUS/$10^{-32}$ dependence with the IACT E$_{\rm th}$. For a given E$_{\rm th}$, the shadow region scans all the $m_\chi$, $\left<\sigma v\right>$ and N$_\gamma$ intervals (see text).