162083.fig.005a
(a)
162083.fig.005b
(b)
Figure 5: (a) The cumulative number of subhalos with flux exceeding , . (b) The fraction of dark clumps, that is, subhalos likely not hosting any stars and defined by ,  km s , or  km s , as a function of limiting flux . These distributions are averages over 100 randomly chosen observer locations 8 kpc from the host halo center.