All Tables

Table 1: Fit results for different spectral models. The differential flux normalisation I₀ and the integral flux above 1 TeV $(I({>}1~{\rm TeV}))$ are given in units of $10^{-12}~{\rm cm}^{-2}~{\rm s}^{-1}~{\rm TeV}^{-1}$ and $10^{-12}~{\rm cm}^{-2}~{\rm s}^{-1}$ , respectively. The power-law fit is clearly an inappropriate description of the data, a power law with an exponential cutoff (row 2), a power law with an energy dependent photon index (row 3), and a broken power law (row 4; in the formula, the parameter S = 0.4 describes the sharpness of the transition from $\Gamma _1$ to $\Gamma _2$ and it is fixed in the fit) are equally likely descriptions of the HESS data. Note that when fitting a broken power law to the data, some of the fit parameters are highly correlated.
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.