We present the first robust helium (He) abundance measurements in star-forming galaxies at redshifts 1. 6 z 3. 3 using deep, moderate-resolution JWST/NIRSpec spectroscopy from the AURORA survey. We establish a High-z HeI Sample consisting of 20 galaxies with multiple high-S/N (>5σ) HeI emission-line detections, including the critical near-infrared λ10833 line. This is the first study at high redshift leveraging λ10833 to break degeneracies between temperature, electron density, optical depth, and He^+/H^+, enabling reliable He abundance determinations in the early universe. We use a custom MCMC framework incorporating direct-method electron temperature priors, extended optical depth (τ₃₈₉₀) model grids up to densities of 10⁶~cm^-3, and simultaneous fits of the physical conditions and HeI/HI line ratios to derive ionic He^+/H^+ abundances. Most of the AURORA galaxies follow the extrapolated z0 He/H-O/H trend, indicating modest He enrichment by z2-3. However, we identify a subpopulation of four galaxies that exhibit elevated He mass fractions (ΔY>0. 03) without corresponding enhancements in N/O or α-elements (20% of the sample). This abundance pattern is inconsistent with enrichment from asymptotic giant branch stars, but favors early He enrichment from very massive stars (VMSs; M100\ M_), which can eject He-rich, N-poor material via stellar winds and binary stripping in young stellar populations. We speculate that these elevated-He systems may represent an early phase of globular cluster (GC) formation where N enrichment is still lagging behind He production. This work demonstrates the power of JWST multi-line HeI spectroscopy for tracing early stellar feedback, enrichment pathways, and GC progenitor signatures in the high-z universe.
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