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We present the first 3D simulations to include the effects of dark matterannihilation feedback during the collapse of primordial mini-halos. We beginour simulations from cosmological initial conditions and account for darkmatter annihilation in our treatment of the chemical and thermal evolution ofthe gas. The dark matter is modelled using an analytical density profile thatresponds to changes in the peak gas density. We find that the gas can collapseto high densities despite the additional energy input from the dark matter. Noobjects supported purely by dark matter annihilation heating are formed in oursimulations. However, we find that the dark matter annihilation heating has alarge effect on the evolution of the gas following the formation of the firstprotostar. Previous simulations without dark matter annihilation found thatprotostellar discs around Population III stars rapidly fragmented, formingmultiple protostars that underwent mergers or ejections. When dark matterannihilation is included, however, these discs become stable to radii of 1000AU or more. In the cases where fragmentation does occur, it is a wide binarythat is formed.

WIMP DM and first stars: suppression of fragmentation in primordial star formation