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Abstract

We describe a population of young star clusters (SCs) formed in a hydrodynamical simulation of a gas-rich dwarf galaxy merger resolved with individual massive stars at sub-parsec spatial resolution. The simulation is part of the GRIFFIN (Galaxy Realizations Including Feedback From INdividual massive stars) project. The star formation environment during the simulation spans seven orders of magnitude in gas surface density and thermal pressure, and the global star formation rate surface density (Σ_SFR) varies by more than three orders of magnitude during the simulation. Young SCs more massive than M_∗,cl∼10^2.5M_⊙ form along a mass function with a power-law index α∼−1.7 (α∼−2 for M_∗,cl ≳10³M_⊙) at all merger phases, while the normalization and the highest SC masses (up to ∼10⁶M_⊙) correlate with Σ_SFR. The cluster formation efficiency varies from Γ∼20% in early merger phases to Γ∼80% at the peak of the starburst and is compared to observations and model predictions. The massive SCs (≳10⁴M_⊙) have sizes and mean surface densities similar to observed young massive SCs. Simulated lower mass clusters appear slightly more concentrated than observed. All SCs form on timescales of a few Myr and lose their gas rapidly resulting in typical stellar age spreads between σ∼0.1−2 Myr (1σ), consistent with observations. The age spreads increase with cluster mass, with the most massive cluster (∼10⁶M_⊙) reaching a spread of 5Myr once its hierarchical formation finishes. Our study shows that it is now feasible to investigate the SC population of entire galaxies with novel high-resolution numerical simulations.