<b>E</b> mission-line Diagnostics at <i>z</i>  &gt; 4: [O <scp>iii</scp> ] <i>λ</i> 4364/H <i>γ</i> versus [Ne <scp>iii</scp> ] <i>λ</i> 3870/[O <scp>ii</scp> ] <i>λ</i> 3730

Abstract We use JWST Near-Infrared Spectrograph observations from the Cosmic Evolution Early Release survey, GLASS-JWST ERS (GLASS), and JWST Advanced Deep Extragalactic Survey to measure rest-frame optical emission-line ratios of 89 galaxies at z &gt; 4. The stacked spectra of galaxies with and without a broad-line feature reveal a difference in the [O iii ] λ 4364 and H γ ratios. This motivated our investigation of the [O iii ] λ 4364/H γ versus [Ne iii ]/[O ii ] diagram. We define two active galactic nucleus (AGN)/star formation (SF) classification lines based on 21,048 Sloan Digital Sky Survey galaxies at z ∼ 0. After applying a redshift correction to the AGN/SF lines, we find 69.2% of broad-line active galactic nuclei (BLAGN) continue to land in the AGN region of the diagnostic, largely due to the [Ne iii ]/[O ii ] ratio. However, 33.0% of non-BLAGN land is in the AGN region as well. The [O iii ] λ 4364/H γ versus [Ne iii ]/[O ii ] diagram does not robustly separate BLAGN from non-broad-line galaxies at z &gt; 4. This could be due to star-forming galaxies having harder ionization, or these galaxies contain a narrow line AGN, which are not accounted for. We further inspected galaxies without broad emission lines in each region of [O iii ] λ 4364/H γ versus [Ne iii ]/[O ii ] diagram and found that they have slightly stronger C iii ] λ 1908 fluxes and equivalent width when landing in the BLAGN region. However, the cause of this higher ionization is unclear and may be revealed by observing UV lines.