CLEAR: High-ionization Ne v λ3426 Emission-line Galaxies at 1.4 < z < 2.3

Abstract We analyze a sample of 25 Ne v ( λ 3426) emission-line galaxies at 1.4 < z < 2.3 using Hubble Space Telescope/Wide Field Camera 3 G102 and G141 grism observations from the CANDELS Ly α Emission at Reionization (CLEAR) survey. Ne v emission probes extremely energetic photoionization (creation potential of 97.11 eV) and is often attributed to energetic radiation from active galactic nuclei (AGNs), shocks from supernovae, or an otherwise very hard ionizing spectrum from the stellar continuum. In this work, we use Ne v in conjunction with other rest-frame UV/optical emission lines (O ii λ λ 3726, 3729, Ne iii λ 3869, H β , O iii λ λ 4959, 5007, H α +N ii λ λ 6548, 6583, S ii λ λ 6716, 6731), deep (2–7 Ms) X-ray observations (from Chandra), and mid-infrared imaging (from Spitzer) to study the origin of this emission and to place constraints on the nature of the ionizing engine. The majority of the Ne v -detected galaxies have properties consistent with ionization from AGNs. However, for our Ne v -selected sample, the X-ray luminosities are consistent with local ( z ≲ 0.1) X-ray-selected Seyferts, but the Ne v luminosities are more consistent with those from z ∼ 1 X-ray-selected QSOs. The excess Ne v emission requires either reduced hard X-rays or a ∼0.1 keV excess. We discuss possible origins of the apparent Ne v excess, which could be related to the “soft (X-ray) excess” observed in some QSOs and Seyferts and/or be a consequence of a complex/anisotropic geometry for the narrow-line region, combined with absorption from a warm, relativistic wind ejected from the accretion disk. We also consider implications for future studies of extreme high-ionization systems in the epoch of reionization ( z ≳ 6) with the James Webb Space Telescope.