Strong He I Emission Lines in High N/O Galaxies at z ∼ 6 Identified in JWST Spectra: High He/H Abundance Ratios or High Electron Densities?

October 2024 • 2024ApJ...974..266Y

Authors • Yanagisawa, Hiroto • Ouchi, Masami • Watanabe, Kuria • Matsumoto, Akinori • Nakajima, Kimihiko • Yajima, Hidenobu • Nagamine, Kentaro • Takahashi, Koh • Nakane, Minami • Tominaga, Nozomu • Umeda, Hiroya • Fukushima, Hajime • Harikane, Yuichi • Isobe, Yuki • Ono, Yoshiaki • Xu, Yi • Zhang, Yechi

Abstract • We present He I/Hβ flux and He/H abundance ratios in three James Webb Space Telescope galaxies with significant constraints on N/O abundance ratios, GS-NDG-9422, RXCJ2248-ID, and GLASS150008 at z ∼ 6 mostly with the spectroscopic coverage from He I λ4471 and He II λ4686 to He I λ7065, and comparing with 68 local dwarf galaxies. We find that these high-z galaxies present strong He I emission with He I/Hβ flux ratios generally larger than those of local dwarf galaxies. We derive He/H with all of the detected HeI, He II, and 2‑3 hydrogen Balmer lines in the same manner as the local He/H determination conducted for cosmology studies. These high-z galaxies show He overabundance He/H ≳0.10 or high electron density of n _e ∼ 10^3‑4 cm^‑3 much larger than local values at low O/H, . In contrast, we obtain low He/H and n _e values for our local dwarf galaxies by the same technique with the same helium and hydrogen lines, and confirm that the difference between the high-z and local dwarf galaxies is not mimicked by systematics. While two scenarios of (1) He overabundance and (2) high electron density are not clearly concluded, we find that there is a positive correlation between the He/H–N/O or n _e–N/O plane by the comparison of the high-z and local dwarf galaxies. Scenario (1) suggests that the overabundant helium and nitrogen are not explained by the standard chemical enrichment of core-collapse supernovae, but by the CNO-cycle products and equilibrium ratios, respectively. Scenario (2) indicates that the strong helium lines originated from the central dense clouds of the high-z galaxies by excessive collisional excitation.

Links

• PREPRINT http://arxiv.org/abs/2405.01823
• ELECTR https://doi.org/10.3847%2F1538-4357%2Fad72ec