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We introduce a new set of zoom-in cosmological simulations with sub-pcresolution, intended to model extremely faint, highly magnified star-formingstellar clumps, detected at z=6.14 thanks to gravitational lensing. Thesimulations include feedback from individual massive stars (in both thepre-supernova and supernova phases), generated via stochastic, direct samplingof the stellar initial mass function. We adopt a modified 'delayed cooling'feedback scheme, specifically created to prevent artificial radiative loss ofthe energy injected by individual stars in very dense gas (n~10^3-10^5cm^{-3}). The sites where star formation ignites are characterised by maximumdensities of the order of 10^5 cm^{-3} and gravitational pressures P/k>10^7K/cm^3, corresponding to the values of the local, turbulent regions where thedensest stellar aggregates form. The total stellar mass at z=6.14 is 3.4x10^7M_sun, in satisfactory agreement with the observed stellar mass of the observedsystems. The most massive clumps have masses of ~10^6 M_sun and half-mass sizesof ~100 pc. These sizes are larger than the observed ones, including also othersamples of lensed high-redshift clumps, and imply an average density one orderof magnitude lower than the observed one. In the size-mass plane, our clumpspopulate a sequence that is intermediate between the ones of observedhigh-redshift clumps and local dSph galaxies.

Sub-parsec resolution cosmological simulations of star-forming clumps at high redshift with feedback of individual stars