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One of the key mysteries of star formation is the origin of the stellarinitial mass function (IMF). The IMF is observed to be nearly universal in theMilky Way and its satellites, and significant variations are only inferred inextreme environments, such as the cores of massive elliptical galaxies. In thiswork we present simulations from the STARFORGE project that are the firstcloud-scale RMHD simulations that follow individual stars and include allrelevant physical processes. The simulations include detailed gasthermodynamics, as well as stellar feedback in the form of protostellar jets,stellar radiation, winds and supernovae. In this work we focus on how stellarradiation, winds and supernovae impact star-forming clouds. Radiative feedbackplays a major role in quenching star formation and disrupting the cloud,however the IMF peak is predominantly set by protostellar jet physics. We findthe effect of stellar winds is minor, and supernovae occur too late}to affectthe IMF or quench star formation. We also investigate the effects of initialconditions on the IMF. The IMF is insensitive to the initial turbulence, cloudmass and cloud surface density, even though these parameters significantlyshape the star formation history of the cloud, including the final starformation efficiency. The characteristic stellar mass depends weakly onmetallicity and the interstellar radiation field. Finally, while turbulentdriving and the level of magnetization strongly influences the star formationhistory, they only influence the high-mass slope of the IMF.

Effects of the environment and feedback physics on the initial mass function of stars in the STARFORGE simulations