The dynamical evolution of the stellar clumps in the Sparkler galaxy

Recent James Webb Space Telescope observations detected a system of stellar clumps around the z≃1.4 gravitationally lensed Sparkler galaxy (of stellar mass M_*∼10^9 with ages and metallicities compatible with globular cluster (GC) progenitors. However, most of their masses (>10⁶ and sizes (>30$ pc) are about ten times those of GCs in the local Universe. To assess whether these clumps can evolve into GC-like objects, we performed N-body simulations of their dynamical evolution from z≃1.4 to z=0 (∼9.23 Gyr) under the effect of dynamical friction and tidal stripping. We studied dynamical friction by performing multiple runs of a system of clumps in a Sparkler-like spherical halo of mass M_ ≃5 that was inferred from the stellar-to-halo mass relation. For the tidal stripping, we simulated resolved clumps orbiting in an external static gravitational potential including the same halo as in the dynamical friction simulations and a Sparkler-like stellar disc. Dynamical friction causes the clumps with a mass greater than $10^7 to sink into the central galaxy regions, possibly contributing to the bulge growth. In absence of tidal stripping, the mass distribution of the surviving clumps (≈40%) peaks at ≈5 implying the presence of uncommonly over-massive clumps at z=0. Tidal shocks from the stellar disc strip considerable mass from low-mass clumps, but their sizes remain larger than those of present-day GCs. When the surviving clumps are corrected for tidal stripping, their mass distribution peak shifts to ∼2 that is compatible with very massive GCs. Our simulations suggest that a fraction of the Sparkler clumps is expected to fall into the central regions, where they might become bulge fossil fragments or contribute to the formation of a nuclear star cluster. The remaining clumps are too large in size to be progenitors of GCs.