The Dark Matter Annihilation Signal from Dwarf Galaxies and Subhalos

Figure 5

(a) The cumulative number of subhalos with flux exceeding ℱ_tot, ℱ_𝑐. (b) The fraction of dark clumps, that is, subhalos likely not hosting any stars and defined by 𝑀_0.3<5×10⁶M_⊙, 𝑉_max<8 km s−1, or 𝑉_peak<14 km s−1, as a function of limiting flux ℱ_tot. These distributions are averages over 100 randomly chosen observer locations 8 kpc from the host halo center.

(a)

(b)