We present the SPARK (Simulation of Pop III in arepo with Radiation and Kinetic feedback) framework, a new $\mathrm{Pop}\mathrm{III}+\text{Pop}\mathrm{II}$ subgrid framework implemented in the moving-mesh code arepo, designed to study the impact of Pop III feedback on star formation in the early Universe. The framework combines primordial nonequilibrium chemistry, metal-line cooling, initial mass function (IMF)-sampled stellar evolution with supernova feedback, and approximate Lyman-Werner (LW) and ionizing radiation transport. We run a suite of $1c\mathrm{Mpc}/h$ box simulations with different initial conditions and resolutions from $z=127$ to $z=10$. The highest gas mass and spatial resolution in the fiducial simulation reach $\sim 10M_{\odot }$ and $\sim 4\mathrm{pc}$, respectively. The model successfully reproduces the Pop II star formation rate density consistent with previous theoretical works across all initial conditions, with minor variations mainly driven by local halo interactions and LW irradiation. We find that the volume filling factor of metal-enriched gas converges to $\sim 0.5–2\%$ at $z=10$, with scatter driven by stochastic and mixing model variations. Convergence is achieved once subhalos with $M_{\text{subhalo}}\gtrsim {10}^{6.5}{M}_{\odot }$ are resolved, and the total stellar mass at $z=10$ is largely insensitive to initial conditions or the resolution considered in this work. A fiducial simulation requires $\sim {10}^4$ CPU hours, making the framework computationally tractable for larger box simulations and enabling future large parameter studies of stellar physics or environment effects such as Pop III IMF variations, x-ray radiation, or the streaming velocity at high redshift.

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• Evolution of the Universe
• Formation & evolution of stars & galaxies
• Intergalactic medium
• Large scale structure of the Universe
• Astronomical masses & mass distributions
• Astrophysical & cosmological simulations