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 ~ 103-105 cm-3). The sites where star formation ignites are characterized by maximum densities of the order of 105 cm-3 and gravitational pressures Pgrav/k >107 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 3.4 ×10^7 M⊙, in satisfactory agreement with the observed stellar mass of the observed systems. The most massive clumps have masses of ∼10^6 M⊙ 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 orders 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.

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

P Rosati;
2022

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 ~ 103-105 cm-3). The sites where star formation ignites are characterized by maximum densities of the order of 105 cm-3 and gravitational pressures Pgrav/k >107 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 3.4 ×10^7 M⊙, in satisfactory agreement with the observed stellar mass of the observed systems. The most massive clumps have masses of ∼10^6 M⊙ 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 orders 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.
2022
Calura, F; Lupi, A; Rosdahl, J; Vanzella, E; Meneghetti, M; Rosati, P; Vesperini, E; Lacchin, E; Pascale, R; Gilli, R
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11392/2504073
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