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The formation of Population III (Pop III) stars is a critical step in theevolution of the early universe. To understand how these stars affected theirmetal-enriched descendants, the details of how, why and where Pop III formationtakes place needs to be determined. One of the processes that is assumed togreatly affect the formation of Pop III stars is the presence of a Lyman-Werner(LW) radiation background, that destroys H$_2$, a necessary coolant in thecreation of Pop III stars. Self-shielding can alleviate the effect the LWbackground has on the H$_2$ within haloes. In this work, we perform acosmological simulation to study the birthplaces of Pop III stars, using theadaptive mesh refinement code Enzo. We investigate the distribution of hosthalo masses and its relationship to the LW background intensity. Compared toprevious work, haloes form Pop III stars at much lower masses, up to a factorof a few, due to the inclusion of H$_2$ self-shielding. We see no relationshipbetween the LW intensity and host halo mass. Most haloes form multiple Pop IIIstars, with a median number of four, up to a maximum of 16, at the instance ofPop III formation. Our results suggest that Pop III star formation may be lessaffected by LW radiation feedback than previously thought and that Pop IIImultiple systems are common.

Cradles of the first stars: self-shielding, halo masses, and multiplicity