All Tables

Table 1: The input parameters of the four mSUGRA benchmark models we consider here. The units for the mass parameters are GeV, and the universal trilinear coupling A₀ is set to 0 for all models (see Battaglia et al. 2004, for details).
Table 2: The branching ratios into various final states for the four mSUGRA benchmark models of Table 1; in the last column we also indicate $\langle\sigma v\rangle_0$ in units of ${\rm cm}^3~{\rm s}^{-1}$ .
Table 3: Predicted flux in various frequency ranges for a neutralino $b\bar b$ model with $M_{\chi } = 40$ GeV and $\langle \sigma v \rangle = 10^{-26}$ cm³/s. The value of the magnetic field is $B_{\mu}=1.2 ~ \mu$ G. E_particle refers to the approximate energy for $e^\pm$ or $\gamma$ sourcing the corresponding flux in the monochromatic limit.
Table 4: Order-of-magnitude estimates of the values of the cross-section, $\langle\sigma v\rangle_0$ , in units of ${\rm cm^3}\ {\rm s^{-1}}$ , needed to reproduce the detected non-thermal emission features in Coma and to produce sizable signals for future indirect dark matter search experiments in the Milky Way.