Astronomy & Astrophysics

Table 1: Fraction of the number of exotic primaries emitted in $V_{\rm PBH}(99\%)$ and $V_{\rm SUSY}(99\%)$ for various L, compared to the total number of exotic primaries emitted either in the bounded geometry (halo size L and radial extension R=20 kpc) - denoted $f^{\rm cyl}(L)$ -, or in the whole dark halo - denoted $f^{\rm tot}(L)$ .
Table 2: Fraction of primaries $f^{{\rm esc}}$ emitted from the (50-90-99)%-volumes of the cylindrical geometry (see above) that escape through upper and lower boundary located at L=10 kpc or L=2 kpc (for PBH and SUSY effective source distribution), before they can reach the Solar neighborhood.
Table 3: $r_{\rm w}$ and $r_{\rm sp}$ for three halo sizes L and three diffusion slopes $\delta$ : these numbers are for 1 GeV/nuc (interstellar energy) antideuterons.
Table 4: The quantity $r_{\rm loss}$ (kpc) is given for three halo sizes L and three diffusion slopes $\delta$ at the total energy E=7 GeV.
Table 5: Summary of the typical cut-off in z and r directions beyond where a cosmic ray cannot originate. The sole parameters that determine these cut-offs are L (halo size) and/or $\chi _{\rm w}\equiv r_{\rm w}/L$ - related to the convective wind $V_{\rm c}$ via $r_{\rm w}=2K/V_{\rm c}$ , or $r_{\rm loss}$ related to the effective life-time for positrons and electrons.