The annihilation rate of weakly interacting cold dark matter particles at the galactic center could be greatly enhanced by the growth of a density spike around the central supermassive black hole (SBH). Here we discuss the effects of hierarchical mergers on the central spike. Mergers between halos containing SBHs lead to the formation of SBH binaries which transfer energy to the dark matter particles, lowering their density. The predicted flux of annihiliation photons from the galactic center is several orders of magnitude smaller than in models that ignore the effects of SBHs and mergers. Measurement of the annihilation radiation could in principle be used to constrain the merger history of the galaxy.The dark matter puzzle is one of the central challenges facing particle physics and cosmology [1]. A popular candidate for non-baryonic cold dark matter (CDM) is the lightest supersymmetric particle, plausibly the neutralino χ [2,3]. The mass of the neutralino is constrained by accelerator searches and theoretical considerations of thermal freeze-out to lie in the range 30GeV < ∼ M χ < ∼ 10TeV [4,5]. Neutralinos are generically found to decouple at a temperature that is roughly M χ /20, which means that they are nonrelativistic already at decoupling and hence behave like CDM.Dark matter particles may be detected directly, via laboratory experiments [6], or indirectly, via their annihilation products [7]. Indirect schemes are typically based on searches for gamma rays from neutralino annihilations in the dark matter halo of the Milky Way (MW) galaxy [8,9,10]. Since the photon flux depends on the squared density of neutralinos integrated along the line of sight, the signal is greatly enhanced in directions where the dark matter is clumped. This includes the galactic center, where the density in a smooth halo would be maximum, as well as any lines of sight intersecting the centers of relic halos that orbit as subclumps in the MW halo [11,12]. The signal from the galactic center is further enhanced if there is a CDM "spike" associated with the central supermassive black hole (SBH). Adiabatic growth of a SBH at the center of a pre-existing halo produces a power-law distribution of matter around the SBH, a "spike," with density; M • is the SBH mass and σ is the 1D velocity dispersion of the dark matter particles. 14,15,16] and r h ∼ 1 pc. These spikes lead to predictions of higherthan-observed rates of γ-ray annihilation products [17].One element missing from earlier discussions of dark matter spikes is the destructive effect of hierarchical mergers. A dark matter halo as massive as that of the MW, M ∼ 10 12 M ⊙ , has almost certainly experienced a significant merger event since a redshift of z ∼ 2. Furthermore, SBHs with masses of ∼ 10 9 M ⊙ were present in at least some halos already at redshifts of 5 − 6 [18,19], and SBHs probably acquired most of their mass by a redshift of 2 − 3, the epoch of peak quasar activity [20]. In the CDM paradigm, big halos grow through the buildup of smaller ones [21]; if more than one of...