| Issue |
A&A
Volume 531, July 2011
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 2 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/20066381e | |
| Published online | 08 June 2011 | |
Primary particle acceleration above 100 TeV in the shell-type supernova remnant RX J1713.7 − 3946 with deep H.E.S.S. observations (Corrigendum)
1
Max-Planck-Institut für Kernphysik, PO Box 103980, 69029 Heidelberg, Germany
e-mail: Christopher.van.Eldik@mpi-hd.mpg.de
2
Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia
3
Centre d’Étude Spatiale des Rayonnements, CNRS/UPS, 9 av. du Colonel Roche, BP 4346, 31029 Toulouse Cedex 4, France
4
Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, 22761 Hamburg, Germany
5
Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, 12489 Berlin, Germany
6
LUTH, UMR 8102 du CNRS, Observatoire de Paris, Section de Meudon, 92195 Meudon Cedex, France
7
DAPNIA/DSM/CEA, CE Saclay, 91191 Gif-sur-Yvette Cedex, France
8
University of Durham, Department of Physics, South Road, Durham DH1 3LE, UK
9
Unit for Space Physics, North-West University, Potchefstroom 2520, South Africa
10
Laboratoire Leprince-Ringuet, IN2P3/CNRS, École Polytechnique, 91128 Palaiseau, France
11
Laboratoire d’Annecy-le-Vieux de Physique des Particules, IN2P3/CNRS, 9 chemin de Bellevue, BP 110, 74941 Annecy-le-Vieux Cedex, France
12
APC, 11 place Marcelin Berthelot, 75231 Paris Cedex 05, France
13 Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland
14
Landessternwarte, Universität Heidelberg, Königstuhl, 69117 Heidelberg, Germany
15
Laboratoire de Physique Théorique et Astroparticules, IN2P3/CNRS, Université Montpellier II, CC 70, Place Eugène Bataillon, 34095 Montpellier Cedex 5, France
16
Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany
17
Laboratoire d’Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France
18
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
19
Laboratoire de Physique Nucléaire et de Hautes Énergies, IN2P3/CNRS, Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 5, France
20 Institute of Particle and Nuclear Physics, Charles University, V Holesovickach 2, 180 00 Prague 8, Czech Republic
21
Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, 44780 Bochum, Germany
22 University of Namibia, Private Bag 13301, Windhoek, Namibia
Key words: acceleration of particles / cosmic rays / gamma rays: observations / ISM: supernova remnants / errata, addenda
 |
Fig. 4 Combined H.E.S.S. gamma-ray spectrum of RX J1713.7−3946 generated from data of 2003, 2004, and 2005 (Data set III, Table 1). Data are corrected for the variation in optical efficiency. Error bars are ± 1σ statistical errors. These data might be described by a power law with exponential cutoff of the form dN/dE = I0 E − Γ exp( − (E/Ec)β). The best-fit result (black solid line) is given here for β = 0.5 (fixed), Γ = 1.8, and Ec = 3.7 TeV (cf. Table 4 for the exact values). Note that the fit function extends as dashed black line beyond the fit range for illustration. For comparison, the best fit of a power law with exponential cutoff and β = 1, obtained solely from the 2004 data (Aharonian et al. 2007), is shown as dashed red line. A model-independent upper limit, indicated by the black arrow, is determined in the energy range from 113 to 300 TeV. |
The differential fluxes given in Table 5 of Aharonian et al. (2007) were overestimated by 19%. When the energy correction factors (discussed in the main text) were originally applied to the spectrum data, no correction was made to the calculation of the differential fluxes for the increased widths of the energy bins. The correct flux values are now given in Table 5. We also note that the incorrect flux units given in the original table have been corrected.
The corresponding flux points plotted in Fig. 4 of Aharonian et al. (2007) are, however, correct, except for the upper limit, which is also overestimated by 19%. Figure 4 shows the differential flux spectrum with the correct upper limit. All other numbers given in Aharonian et al. (2007), including the fit parameters given in Table 4, are unaffected.
References
- Aharonian et al. (H.E.S.S. Collaboration) 2006, A&A, 449, 223 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Aharonian et al. (H.E.S.S. Collaboration) 2007, A&A, 464, 235 [Google Scholar]
- Li, T.-P., & Ma, Y.-Q. 1983, ApJ, 272, 317 [NASA ADS] [CrossRef] [Google Scholar]
© ESO, 2011
All Tables
All Figures
|
Fig. 4 Combined H.E.S.S. gamma-ray spectrum of RX J1713.7−3946 generated from data of 2003, 2004, and 2005 (Data set III, Table 1). Data are corrected for the variation in optical efficiency. Error bars are ± 1σ statistical errors. These data might be described by a power law with exponential cutoff of the form dN/dE = I0 E − Γ exp( − (E/Ec)β). The best-fit result (black solid line) is given here for β = 0.5 (fixed), Γ = 1.8, and Ec = 3.7 TeV (cf. Table 4 for the exact values). Note that the fit function extends as dashed black line beyond the fit range for illustration. For comparison, the best fit of a power law with exponential cutoff and β = 1, obtained solely from the 2004 data (Aharonian et al. 2007), is shown as dashed red line. A model-independent upper limit, indicated by the black arrow, is determined in the energy range from 113 to 300 TeV. |
| In the text | |
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