Table 2: Fit results for distinct regions of the SNR. Given are for each region the photon index resulting from a power-law fit, the best-fit $\chi ^2$ and the number of degrees of freedom (d.o.f.), the integral flux above 1 TeV and the significance of the excess events in units of standard deviation $(\sigma )$. The background for each region was determined from the same field of view, as described in Sect. 2.5.2, for each region separately, and hence the background estimates for different regions are not independent. The first row is the fit result of the whole SNR for comparison. For the whole table, the upper fit range was restricted to 8 TeV to avoid biases due to the deviation from a power law at high energies.
Region $\Gamma$ $\chi ^2$ (d.o.f.) $I({>}1~{\rm TeV})$ Excess
      $(10^{-12}~{\rm cm}^{-2}~{\rm s}^{-1})$ $(\sigma )$
All $2.12 \pm 0.03$ 24.5 (18) $15.9 \pm 0.6$ 30.8
1 $2.12 \pm 0.07$ 34.7 (18) $1.05 \pm 0.13$ 12.9
2 $2.24 \pm 0.06$ 26.0 (17) $1.34 \pm 0.10$ 17.2
3 $2.11 \pm 0.06$ 30.2 (18) $1.45 \pm 0.13$ 16.7
4 $2.10 \pm 0.08$ 15.7 (18) $1.06 \pm 0.12$ 11.5
5 $2.09 \pm 0.07$ 12.6 (18) $1.22 \pm 0.11$ 13.3
6 $2.13 \pm 0.06$ 35.7 (17) $1.23 \pm 0.12$ 14.1
7 $1.95 \pm 0.08$ 9.4 (16) $1.19 \pm 0.12$ 10.9
8 $2.11 \pm 0.12$ 13.8 (14) $0.78 \pm 0.11$ 8.0
9 $2.11 \pm 0.10$ 12.5 (16) $0.89 \pm 0.11$ 8.7
10 $2.19 \pm 0.07$ 24.8 (17) $1.09 \pm 0.10$ 14.1
11 $2.08 \pm 0.08$ 11.6 (15) $1.13 \pm 0.11$ 11.8
12 $2.01 \pm 0.11$ 8.4 (16) $0.81 \pm 0.12$ 8.2
13 $1.98 \pm 0.10$ 10.7 (15) $1.00 \pm 0.14$ 9.8
14 $2.08 \pm 0.11$ 9.9 (15) $0.84 \pm 0.12$ 9.4


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