The Dark Matter Annihilation Signal from Dwarf Galaxies and Subhalos

Figure 3

The annihilation flux ℱ_tot from subhalos in the Via Lactea II simulation versus their 𝑀_0.3, 𝑉_max, and 𝑉_peak. The gray shaded areas indicate regions containing subhalos with ℱ_tot as least as high as the fifth-brightest Milky Way dSph galaxy (Carina), but with 𝑀_0.3<5×10⁶M_⊙, 𝑉_max<8 km s−1, and 𝑉_peak<14 km s−1, that is, probable dark clumps. Only one of the 100 random observer locations used in the analysis is shown here. The number 𝑁_dark in the top left refers to the number of “dark clumps’’ for this particular observer location.

(a)

(b)

(c)