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

TL;DR

This paper presents high-resolution cosmological simulations of star-forming clumps at high redshift, incorporating detailed feedback from individual stars, to better understand the properties and formation of these early universe structures.

Contribution

The study introduces a novel simulation approach with sub-parsec resolution and stochastic stellar feedback, accurately modeling faint, magnified star-forming clumps at z=6.14.

Findings

Simulated stellar mass at z=6.14 matches observations.

Clump sizes are larger and densities lower than observed, indicating model limitations.

Clumps occupy an intermediate size-mass sequence between high-redshift and local dwarf galaxies.

Abstract

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