{
  "id": "2209.06247",
  "version": "v1",
  "published": "2022-09-13T18:08:33.000Z",
  "updated": "2022-09-13T18:08:33.000Z",
  "title": "CLEAR: High-Ionization [Ne V] $λ$3426 Å Emission-line Galaxies at $1.4 <z< 2.3$",
  "authors": [
    "Nikko J. Cleri",
    "Guang Yang",
    "Casey Papovich",
    "Jonathan R. Trump",
    "Bren E. Backhaus",
    "Vicente Estrada-Carpenter",
    "Steven L. Finkelstein",
    "Mauro Giavalisco",
    "Taylor A. Hutchison",
    "Zhiyuan Ji",
    "Intae Jung",
    "Jasleen Matharu",
    "Ivelina Momcheva",
    "Grace M. Olivier",
    "Raymond Simons",
    "Benjamin Weiner"
  ],
  "comment": "17 pages + 2 (appendix), 8 figures + 2(appendix)",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We analyze a sample of 25 [Ne V] (${\\lambda}$3426 $\\r{A}$) 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 Lyman-${\\alpha}$ 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 (AGN), radiative supernova shocks, 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] ${\\lambda\\lambda}$3726,3729 $\\r{A}$, [Ne III] ${\\lambda}$3869 $\\r{A}$, [O III] ${\\lambda\\lambda}$4959,5007 $\\r{A}$, H${\\alpha}$+[N II] ${\\lambda\\lambda}$6548,6583 $\\r{A}$, [S II] ${\\lambda\\lambda}$6716,6731 $\\r{A}$), 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 AGN. 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.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-09-13T18:08:33.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "emission-line galaxies",
      "high-ionization",
      "james webb space telescope"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 17,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}