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.
  Cuspy profile Cored profile

Coma cluster		 $\langle\sigma v\rangle_0$ ( ${\rm cm^3}\ {\rm s^{-1}}$) $\langle\sigma v\rangle_0$ ( ${\rm cm^3}\ {\rm s^{-1}}$)

Radio		 $5 \times 10^{-25}$ $5 \times 10^{-24}$
EUV $3 \times 10^{-23}$ $3 \times 10^{-22}$
HXR $2.5 \times 10^{-23}$ $2.5 \times 10^{-22}$
$\gamma $-ray (EGRET limit) $1.3 \times 10^{-23}$ $1.3 \times 10^{-22}$
$\gamma $-ray (GLAST limit) $7.5 \times 10^{-25}$ $7.5 \times 10^{-24}$

Milky Way		 $\langle\sigma v\rangle_0$ ( ${\rm cm^3}\ {\rm s^{-1}}$) $\langle\sigma v\rangle_0$ ( ${\rm cm^3}\ {\rm s^{-1}}$)
Positrons ${\sim} 10^{-26}$ ${\sim} 10^{-25}$
Antiprotons ${\sim} 10^{-27}$ ${\sim} 10^{-26}$
Antideuterons ${\sim} 10^{-27}$ ${\sim} 10^{-26}$
$\gamma $-ray (GLAST limit) ${\sim} 10^{-28}$ ${\sim} 10^{-23}$


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