Figure 3: The annihilation flux from subhalos in the Via Lactea II simulation versus their , , and . The gray shaded areas indicate regions containing subhalos with as least as high as the fifth-brightest Milky Way dSph galaxy (Carina), but with ,  km s , and  km s , that is, probable dark clumps. Only one of the 100 random observer locations used in the analysis is shown here. The number in the top left refers to the number of “dark clumps’’ for this particular observer location.