Feedback-Free Star Formation in Clusters within a Galaxy Simulated at High Resolution in Cosmic Dawn

Abstract We perform a cosmological zoom-in simulation of a massive galaxy ($M_s\sim 10^{10}\rm M_\odot$ at z ∼ 10) using the GIZMO code. By employing $\le 3\rm pc$ resolution and a $3.4\rm Myr$ supernova feedback delay, we capture the feedback-free starbursts (FFB) in clusters. The simulation reproduces FFB model predictions and super-bright galaxies observed by JWST. At z ∼ 10, cold streams feed a compact galaxy ($R_{\rm e}\sim 1\rm kpc$), with stellar and surface densities ($>10^5\rm cm^{-3}$, $>10^5\rm M_\odot pc^{-2}$) exceeding FFB thresholds. The global star-formation efficiency (SFE) is ϵs ∼ 0.2–0.3, associated with a fluctuating star-formation history. We identified over 105 star clusters ($M_{\star }>10^{4.5}\rm M_\odot$) with a nearly scale-free mass distribution (dN/dlog M∝M−1.06). Approximately 90% of star formation occurs in clusters, which at a given time constitute $30\!-\!40~{{\ \rm per\ cent}}$ of the total stellar mass. The star formation in most of the clusters of masses $<10^7\rm M_\odot$, occurs in bursts of $<3\rm Myr$ and a local SFE ∼0.5 ± 0.2. Cluster metallicities (−2.01 < log (Z/Z⊙) < −0.45) indicate rapid baryon recycling. Feedback-driven outflows exhibit typical temperature of $10^7\rm K$ and typical velocities of $\sim 2000\rm km\ s^{-1}$. In the highly dynamic central $1\rm kpc$, clusters undergo rapid orbital decay and merge to assemble the oblate nuclear stellar cluster. Cluster shapes range from oblate to prolate, with a triaxial median. These clusters are consistent with JWST observations, and a fraction of them may survive to yield the globular clusters (GCs) at low redshifts.