2026ApJ...996...68B

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 He sample consisting of 20 galaxies with multiple high-signal-to-noise-ratio (>5σ) He I 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 Markov Chain Monte Carlo framework incorporating direct-method electron temperature priors, extended optical depth (τ_λ3890) model grids up to densities of 10⁶ cm^–3, and simultaneous fits of the physical conditions and He I/H I line ratios to derive ionic He⁺/H⁺ abundances. Most of the AURORA galaxies follow the extrapolated z ∼ 0 He/H-O/H trend, indicating modest He enrichment by z ∼ 2-3. 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 (M ≳ 100M_⊙), 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 He I spectroscopy for tracing early stellar feedback, enrichment pathways, and GC progenitor signatures in the high-redshift Universe.