posted on 2019-09-18, 11:23authored byH Abdalla, A Abramowski, F Aharonian, FA Benkhali, EO Anguner, M Arakawa, C Armand, M Arrieta, M Backes, A Balzer, M Barnard, Y Becherini, JB Tjus, D Berge, S Bernhard, K Bernloehr, R Blackwell, M Bottcher, C Boisson, J Bolmont, S Bonnefoy, P Bordas, J Bregeon, F Brun, P Brun, M Bryan, M Buechele, T Bulik, M Capasso, S Caroff, A Carosi, S Casanova, M Cerruti, N Chakraborty, RCG Chaves, A Chen, J Chevalier, S Colafrancesco, B Condon, J Conrad, ID Davids, J Decock, C Deil, J Devin, P deWilt, L Dirson, A Djannati-Atai, A Donath, LO Drury, J Dyks, T Edwards, K Egberts, G Emery, J-P Ernenwein, S Eschbach, C Farnier, S Fegan, M Fernandes, A Fiasson, G Fontaine, S Funk, M Fuessling, S Gabici, YA Gallant, T Garrigoux, F Gate, G Giavitto, D Glawion, JF Glicenstein, D Gottschall, M-H Grondin, J Hahn, M Haupt, J Hawkes, G Heinzelmann, G Henri, G Hermann, JA Hinton, W Hofmann, C Hoischen, TL Holch, M Holler, D Horns, A Ivascenko, H Iwasaki, A Jacholkowska, M Jamrozy, D Jankowsky, F Jankowsky, M Jingo, L Jouvin, I Jung-Richardt, MA Kastendieck, K Katarzynski, M Katsuragawa, U Katz, D Kerszberg, D Khangulyan, B Khelifi, J King, S Klepser, D Klochkov, W Kluzniak, N Komin, K Kosack, S Krakau, M Kraus, PP Kruger, H Laffon, G Lamanna, J Lau, J Lefaucheur, A Lemiere, M Lemoine-Goumard, J-P Lenain, E Leser, T Lohse, M Lorentz, R Liu, R Lopez-Coto, I Lypova, D Malyshev, V Marandon, A Marcowith, C Mariaud, R Marx, G Maurin, N Maxted, M Mayer, PJ Meintjes, M Meyer, AMW Mitchell, R Moderski, M Mohamed, L Mohrmann, K Mora, E Moulin, T Murach, S Nakashima, M de Naurois, H Ndiyavala, F Niederwanger, J Niemiec, L Oakes, P O'Brien, H Odaka, S Ohm, M Ostrowski, I Oya, M Padovani, M Panter, RD Parsons, NW Pekeur, G Pelletier, C Perennes, P-O Petrucci, B Peyaud, Q Piel, S Pita, V Poireau, DA Prokhorov, H Prokoph, G Puehlhofer, M Punch, A Quirrenbach, S Raab, R Rauth, A Reimer, O Reimer, M Renaud, R de los Reyes, F Rieger, L Rinchiuso, C Romoli, G Rowell, B Rudak, CB Rulten, V Sahakian, S Saito, DA Sanchez, A Santangelo, M Sasaki, R Schlickeiser, F Schussler, A Schulz, U Schwanke, S Schwemmer, M Seglar-Arroyo, AS Seyffert, N Shafi, I Shilon, K Shiningayamwe, R Simoni, H Sol, F Spanier, M Spir-Jacob, L Stawarz, R Steenkamp, C Stegmann, C Steppa, I Sushch, T Takahashi, J-P Tavernet, T Tavernier, AM Taylor, R Terrier, L Tibaldo, D Tiziani, M Tluczykont, C Trichard, M Tsirou, N Tsuji, R Tuffs, Y Uchiyama, DJ van der Walt, C van Eldik, C van Rensburg, B van Soelen, G Vasileiadis, J Veh, C Venter, A Viana, P Vincent, J Vink, F Voisin, HJ Voelk, T Vuillaume, Z Wadiasingh, SJ Wagner, P Wagner, RM Wagner, R White, A Wierzcholska, P Willmann, A Woernlein, D Wouters, R Yang, D Zaborov, M Zacharias, R Zanin, AA Zdziarski, A Zech, F Zefi, A Ziegler, J Zorn, N Zywucka, JD Magill, S Buson, CC Cheung, JS Perkins, Y Tanaka
Centaurus A (Cen A) is the nearest radio galaxy discovered as a very-high-energy (VHE; 100 GeV–100 TeV) γ-ray source by the High Energy
Stereoscopic System (H.E.S.S.). It is a faint VHE γ-ray emitter, though its VHE flux exceeds both the extrapolation from early Fermi-LAT observations as well as expectations from a (misaligned) single-zone synchrotron-self Compton (SSC) description. The latter satisfactorily reproduces
the emission from Cen A at lower energies up to a few GeV. New observations with H.E.S.S., comparable in exposure time to those previously
reported, were performed and eight years of Fermi-LAT data were accumulated to clarify the spectral characteristics of the γ-ray emission from
the core of Cen A. The results allow us for the first time to achieve the goal of constructing a representative, contemporaneous γ-ray core spectrum
of Cen A over almost five orders of magnitude in energy. Advanced analysis methods, including the template fitting method, allow detection in
the VHE range of the core with a statistical significance of 12σ on the basis of 213 hours of total exposure time. The spectrum in the energy range
of 250 GeV–6 TeV is compatible with a power-law function with a photon index Γ = 2.52 ± 0.13stat ± 0.20sys. An updated Fermi-LAT analysis
provides evidence for spectral hardening by ∆Γ ' 0.4 ± 0.1 at γ-ray energies above 2.8
+1.0
−0.6 GeV at a level of 4.0σ. The fact that the spectrum
hardens at GeV energies and extends into the VHE regime disfavour a single-zone SSC interpretation for the overall spectral energy distribution
(SED) of the core and is suggestive of a new γ-ray emitting component connecting the high-energy emission above the break energy to the one
observed at VHE energies. The absence of significant variability at both GeV and TeV energies does not yet allow disentanglement of the physical
nature of this component, though a jet-related origin is possible and a simple two-zone SED model fit is provided to this end.
Funding
The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is
gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research
Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt
Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and
CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the U.K. Science and Technology Facilities Council (STFC), the
Knut and Alice Wallenberg Foundation, the National Science Centre, Poland
grant no. 2016/22/M/ST9/00382, the South African Department of Science and
Technology and National Research Foundation, the University of Namibia,
the National Commission on Research, Science & Technology of Namibia
(NCRST), the Austrian Federal Ministry of Education, Science and Research
and the Austrian Science Fund (FWF), the Australian Research Council (ARC),
the Japan Society for the Promotion of Science, and by the University of Amsterdam. We appreciate the excellent work of the technical support staff in Berlin,
Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen, and in Namibia in the
construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national
resource providers of the EGI Federation. Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that
have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à
l’Énergie Atomique and the Centre National de la Recherche Scientifique/Institut
National de Physique Nucléaire et de Physi
History
Citation
Astronomy and Astrophysics, 2018, 619, A71
Author affiliation
/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy
Version
VoR (Version of Record)
Published in
Astronomy and Astrophysics
Publisher
EDP Sciences for European Southern Observatory (ESO)