{
  "id": "0906.5574",
  "version": "v2",
  "published": "2009-06-30T16:17:33.000Z",
  "updated": "2009-07-06T18:45:08.000Z",
  "title": "Detection of very-high-energy gamma-ray emission from the vicinity of PSR B1706-44 with H.E.S.S",
  "authors": [
    "S. Hoppe",
    "E. de Oña-Wilhemi",
    "B. Khélifi",
    "R. C. G. Chaves",
    "O. C. de Jager",
    "C. Stegmann",
    "R. Terrier",
    "for the H. E. S. S. Collaboration"
  ],
  "comment": "4+ pages, 2 figures; v1 submitted to ICRC Proceedings on 15 May 2009; v2 has additional references and minor changes",
  "categories": [
    "astro-ph.HE",
    "astro-ph.GA"
  ],
  "abstract": "The energetic pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G 343.1-2.3 were observed by H.E.S.S. during a dedicated observational campaign in 2007. A new source of very-high-energy (VHE; E > 100 GeV) gamma-ray emission, HESS J1708-443, was discovered with its centroid at RA(J2000) = 17h08m10s and Dec(J2000) = -44d21', with a statistical error of 3 arcmin on each axis. The VHE gamma-ray source is significantly more extended than the H.E.S.S. point-spread function, with an intrinsic Gaussian width of 0.29 +/- 0.04 deg. Its energy spectrum can be described by a power law with a photon index Gamma = 2.0 +/- 0.1 (stat) +/- 0.2 (sys). The integral flux measured between 1-10 TeV is ~17% of the Crab Nebula flux in the same energy range. The possible associations with PSR B1706-44 and SNR G343.1-2.3 are discussed.",
  "revisions": [
    {
      "version": "v2",
      "updated": "2009-07-06T18:45:08.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "very-high-energy gamma-ray emission",
      "energetic pulsar psr",
      "adjacent supernova remnant",
      "crab nebula flux",
      "photon index gamma"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 824459,
      "adsabs": "2009arXiv0906.5574H"
    }
  }
}