Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{ms3378_f3.eps}\end{figure}$ Figure 1: Schematic view of our Galaxy: diffusive and convective propagation plus spallations in the thin disk. Effective primary exotic sources follow either the dark matter profile or its square (isothermal profile is depicted).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3378_f1.eps} \end{figure}$ Figure 2: Isodensity surfaces in the (r,z) plane for L=5 kpc and L=10 kpc (side boundary R=20 kpc). Inner contours correspond to ${\rm d}{\cal P}(r_{\rm s},z_{\rm s}\vert O)/{\rm d}^3\vec{r}_{\rm s}=0.01 ~ \mbox{kpc}^{-3}$ and the contours are spaced by a factor 1/4. From top to bottom, $r_{\rm sp}=3.17$ kpc (no wind), no wind and no spallations, $r_{\rm w}=2.935$ kpc (no spallations). These numbers correspond, respectively, for a reasonable choice of K(E) at 1 GeV, to $\sigma _{\rm sp}\approx 100$ mb and $V_{\rm c}\approx 20$ kpc Myr^-1. The additional thick line in each panel delimitates contours ${\cal P}({\cal V}(f)\vert O)=99\%$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3378_f2.eps}\end{figure}$ Figure 3: Effective source weight (PBH or SUSY) for several profiles (see text).
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{ms3378_f4.eps} \end{figure}$ Figure 4: Contours ${\cal P}({\cal V_{\rm SUSY,~PBH}}\vert R_\odot)=99\%$ origin for L=2, L=5 and L=10 kpc. f-volumes have been respectively evaluated with weight $w_{\rm PBH}(r,z)\propto h_{\rm DM}(r,z)$ (solid lines) and $w_{\rm SUSY}(r,z)\propto h^2_{\rm DM}(r,z)$ (dashed lines) for $R\gg L$ , but the results remain mostly unchanged using R=20 kpc (but in case of a halo size L=10 kpc that requires R=30 kpc). Upper panel: $V_{\rm SUSY}(99\%)$ and $V_{\rm PBH}(99\%)$ in the $x_{\rm s}-y_{\rm s}$ plane ( $z_{\rm s}=0$ ). Lower panel: same quantities but in the $x_{\rm s}-z_{\rm s}$ plane ( $y_{\rm s}=0$ ). In both panels, the dot marks the Galactic center, and $\odot$ denotes the Sun location (it is set to $R_\odot =8$ kpc).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3378_f5.eps}\end{figure}$ Figure 5: Left panel: evolution of $r_{\rm w}$ as a function of kinetic energy per nucleus for primary $\bar{p}$ and $\bar{d}$ ; from top to bottom, $\delta =0.35$ , $\delta =0.60$ and $\delta =0.85$ . The parameter $r_{\rm w}/L\equiv \chi _{\rm w}$ , as well as $r_{\rm sp}/L\equiv \chi _{\rm sp}$ , are not very sensitive to the halo size L (for $\bar{d}$ , only L=6 kpc is displayed) but $r_{\rm w}$ and $r_{\rm sp}$ do. Right panel: $r_{\rm sp}/L$ as a function of E_k/nuc for the same $\delta$ values and for the halo size L=6 kpc. The values of $r_{\rm w}$ are different between $\bar{p}$ and $\bar{d}$ because they depend on rigidity (through K), i.e. on Z/A (it is 1 for $\bar{p}$ and 1/2 for $\bar{d}$ ). For $r_{\rm sp}$ , there is an additional strong dependence on the species because of the destruction cross sections.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3378_f6.eps}\end{figure}$ Figure 6: 99%-volumes for exotic primaries (no side boundaries). Upper panels: cut in the $z_{\rm s}=0$ kpc plane; lower panels: cut in the $y_{\rm s}=0$ kpc plane. Left panels correspond to L=2 kpc, middle panels to L=6 kpc and right panels to L=10 kpc. In each panel, we plot either the PBH case (solid lines) or the SUSY case (dotted lines). From external lines to internal lines correspond the values of the diffusion coefficient slope $\delta =0.35$ , $\delta =0.60$ , $\delta =0.85$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3378_f7.eps}\end{figure}$ Figure 7: ${\cal P}_{\rm cyl}({\cal V}(f)\vert O)=10\%-25\%-50\%-75\%$ for L=10 kpc in the $z_{\rm s}=0$ plane (except for the 75%-volumes, other f-volumes with $f\lesssim 50$ % are not deformed by the boundaries so that they present symmetry around the $x_{\rm s}$ axis). Upper panels correspond to $\delta =0.85$ , and lower panels to $\delta =0.35$ . Both the PBH case (solid lines) and the SUSY case (dotted lines) are plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{ms3378_f3.eps}\end{figure}$	Figure 1: Schematic view of our Galaxy: diffusive and convective propagation plus spallations in the thin disk. Effective primary exotic sources follow either the dark matter profile or its square (isothermal profile is depicted).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3378_f2.eps}\end{figure}$	Figure 3: Effective source weight (PBH or SUSY) for several profiles (see text).
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