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@ARTICLE{Collaboration:165666,
      author       = {Abramowski, A. and Acero, F. and Akhperjanian, A. G. and
                      Anton, G. and Balenderan, S. and Balzer, A. and Barnacka, A.
                      and Becherini, Y. and Tjus, J. Becker and Behera, B. and
                      Bernlöhr, K. and Birsin, E. and Biteau, J. and Bochow, A.
                      and Boisson, C. and Bolmont, J. and Bordas, P. and Brucker,
                      J. and Brun, F. and Brun, P. and Bulik, T. and Carrigan, S.
                      and Casanova, S. and Cerruti, M. and Chadwick, P. M. and
                      Chaves, R. C. G. and Cheesebrough, A. and Colafrancesco, S.
                      and Cologna, G. and Conrad, J. and Couturier, C. and Dalton,
                      M. and Daniel, M. K. and Davids, I. D. and Degrange, B. and
                      Deil, C. and deWilt, P. and Dickinson, H. J. and
                      Djannati-Ataï, A. and Domainko, W. and Drury, L. O'C. and
                      Dubus, G. and Dutson, K. and Dyks, J. and Dyrda, M. and
                      Egberts, K. and Eger, P. and Espigat, P. and Fallon, L. and
                      Farnier, C. and Fegan, S. and Feinstein, F. and Fernandes,
                      M. V. and Fernandez, D. and Fiasson, A. and Fontaine, G. and
                      Förster, A. and Füßling, M. and Gajdus, M. and Gallant,
                      Y. A. and Garrigoux, T. and Gast, H. and Giebels, B. and
                      Glicenstein, J. F. and Glück, B. and Göring, D. and
                      Grondin, M. -H. and Grudzińska, M. and Häffner, S. and
                      Hague, J. D. and Hahn, J. and Hampf, D. and Harris, J. and
                      Heinz, S. and Heinzelmann, G. and Henri, G. and Hermann, G.
                      and Hillert, A. and Hinton, J. A. and Hofmann, W. and
                      Hofverberg, P. and Holler, M. and Horns, D. and
                      Jacholkowska, A. and Jahn, C. and Jamrozy, M. and Jung, I.
                      and Kastendieck, M. A. and Katarzynski, K. and Katz, U. and
                      Kaufmann, S. and Khélifi, B. and Klepser, S. and Klochkov,
                      D. and Kluźniak, W. and Kneiske, T. and Kolitzus, D. and
                      Komin, Nu. and Kosack, K. and Kossakowski, R. and Krayzel,
                      F. and Krüger, P. P. and Laffon, H. and Lamanna, G. and
                      Lefaucheur, J. and Lemoine-Goumard, M. and Lenain, J. -P.
                      and Lennarz, D. and Lohse, T. and Lopatin, A. and Lu, C. -C.
                      and Marandon, V. and Marcowith, A. and Masbou, J. and
                      Maurin, G. and Maxted, N. and Mayer, M. and McComb, T. J. L.
                      and Medina, M. C. and Méhault, J. and Menzler, U. and
                      Moderski, R. and Mohamed, M. and Moulin, E. and Naumann, C.
                      L. and Naumann-Godo, M. and de Naurois, M. and Nedbal, D.
                      and Nguyen, N. and Niemiec, J. and Nolan, S. J. and Ohm, S.
                      and Wilhelmi, E. de $O\$ na and Opitz, B. and Ostrowski, M.
                      and Oya, I. and Panter, M. and Parsons, R. D. and Arribas,
                      M. Paz and Pekeur, N. W. and Pelletier, G. and Perez, J. and
                      Petrucci, P. -O. and Peyaud, B. and Pita, S. and Pühlhofer,
                      G. and Punch, M. and Quirrenbach, A. and Raab, S. and Raue,
                      M. and Reimer, A. and Reimer, O. and Renaud, M. and Reyes,
                      R. de los and Rieger, F. and Ripken, J. and Rob, L. and
                      Rosier-Lees, S. and Rowell, G. and Rudak, B. and Rulten, C.
                      B. and Sahakian, V. and Sanchez, D. A. and Santangelo, A.
                      and Schlickeiser, R. and Schulz, A. and Schwanke, U. and
                      Schwarzburg, S. and Schwemmer, S. and Sheidaei, F. and
                      Skilton, J. L. and Sol, H. and Spengler, G. and Stawarz, Ł.
                      and Steenkamp, R. and Stegmann, C. and Stinzing, F. and
                      Stycz, K. and Sushch, I. and Szostek, A. and Tavernet, J.
                      -P. and Terrier, R. and Tluczykont, M. and Trichard, C. and
                      Valerius, K. and van Eldik, C. and Vasileiadis, G. and
                      Venter, C. and Viana, A. and Vincent, P. and Völk, H. J.
                      and Volpe, F. and Vorobiov, S. and Vorster, M. and Wagner,
                      S. J. and Ward, M. and White, R. and Wierzcholska, A. and
                      Wouters, D. and Zacharias, M. and Zajczyk, A. and Zdziarski,
                      A. A. and Zech, A. and Zechlin, H. -S. and Pelat, D.},
      collaboration = {H.E.S.S.{ Collaboration}},
      title        = {{D}iscovery of {T}e{V} gamma-ray emission from {PKS}
                      0447-439 and derivation of an upper limit on its redshift},
      reportid     = {DESY-2014-00632, arXiv:1303.1628},
      year         = {2013},
      note         = {14 pages, 10 figures, accepted for publication in $A\&A$},
      abstract     = {Very high-energy gamma-ray emission from PKS 0447-439 was
                      detected with the H.E.S.S. Cherenkov telescope array in
                      December 2009. This blazar is one of the brightest
                      extragalactic objects in the Fermi Bright Source List and
                      has a hard spectrum in the MeV to GeV range. In the TeV
                      range, a photon index of 3.89 +- 0.37 (stat) +- 0.22 (sys)
                      and a flux normalisation at 1 TeV, Phi(1 TeV) = (3.5 +- 1.1
                      (stat) +- 0.9 (sys)) x $10^{-13}$ $cm^{-2}$ $s^{-1}$
                      $TeV^{-1},$ were found. The detection with H.E.S.S.
                      triggered observations in the X-ray band with the Swift and
                      RXTE telescopes. Simultaneous UV and optical data from Swift
                      UVOT and data from the optical telescopes ATOM and ROTSE are
                      also available. The spectrum and light curve measured with
                      H.E.S.S. are presented and compared to the multi-wavelength
                      data at lower energies. A rapid flare is seen in the Swift
                      XRT and RXTE data, together with a flux variation in the UV
                      band, at a time scale of the order of one day. A firm upper
                      limit of z < 0.59 on the redshift of PKS 0447-439 is derived
                      from the combined Fermi-LAT and H.E.S.S. data, given the
                      assumptions that there is no upturn in the intrinsic
                      spectrum above the Fermi-LAT energy range and that
                      absorption on the Extragalactic Background Light (EBL) is
                      not weaker than the lower limit provided by current models.
                      The spectral energy distribution is well described by a
                      simple one-zone Synchrotron Self-Compton (SSC) scenario, if
                      the redshift of the source is less than z <~ 0.4.},
      cin          = {ZEU-EXP/AT},
      cid          = {$I:(DE-H253)ZEU-EXP_AT-20120731$},
      pnm          = {523 - High-energy gamma ray astronomy (POF2-523)},
      pid          = {G:(DE-HGF)POF2-523},
      experiment   = {EXP:(DE-MLZ)NOSPEC-20140101},
      typ          = {PUB:(DE-HGF)25 / PUB:(DE-HGF)15},
      eprint       = {1303.1628},
      howpublished = {arXiv:1303.1628},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:1303.1628;\%\%$},
      url          = {https://bib-pubdb1.desy.de/record/165666},
}