2025ApJ...992L..27T

We use the narrow [Ne v] λ3427 emission line detected in the recently published JWST spectra of two galaxies, at z ≃ 6.9 and 5.6, to study the key properties of the active galactic nuclei (AGN) and the supermassive black holes (SMBHs) in their centers. Using a new empirical scaling linking the $\left[{\rm{Ne}}\,{\rm\small{V}}\right]$ line emission with AGN accretion-driven (continuum) emission, derived from a highly complete low-redshift AGN sample, we show that the $\left[{\rm{Ne}}\,{\rm\small{V}}\right]$ emission in the two z > 5 galaxies implies total (bolometric) AGN luminosities of order L_bol ≈ (4-8) × 10⁴⁵ erg s^–1. Assuming that the radiation emitted from these systems is Eddington limited, the (minimal) black hole (BH) masses are of order M_BH ≳ 10⁷M_⊙. Combined with the published stellar masses of the galaxies, estimated from dedicated fitting of their spectral energy distributions, the implied BH-to-stellar mass ratios are of order M_BH/M_host ≈ 0.1-1. This is considerably higher than what is found in the local Universe, but is consistent with the general trend seen in some other z ≳ 5 AGN. Given the intrinsic weakness of the $\left[{\rm{Ne}}\,{\rm\small{V}}\right]$ line and the nature of the $\left[{\rm{Ne}}\,{\rm\small{V}}\right]$-to-L_bol scaling, any (rare) detection of the [Ne v] λ3427 line at z > 5 would translate to similarly high AGN luminosities and SMBH masses, thus providing a unique observational path for studying luminous AGN well into the epoch of reionization, including obscured sources.