data points. Possible VHE $\gamma$-ray variations on a comparable level are below the sensitivity of MAGIC on the given timescale. For each of the three observation periods photon spectra were determined. These are well described by simple power laws between 140 GeV and at least 1.0 TeV and are, within errors, compatible with no change in the spectral index. Finally, all data were combined for the calculation of a differential photon spectrum (Table \[tab:spd\]). The reconstructed spectrum after unfolding with the instrumental energy resolution [@Anykeev1991; @Mizobuchi] is shown in Figure \[fig:spectrum\]. A simple power law fit to the data between 140 GeV and 5.4 TeV yields $$\frac{\mathrm{d}N}{\mathrm{d}E} =
\frac{(1.2\pm0.1_{\mathrm{stat}}\pm{0.5_\mathrm{syst}}) \cdot
10^{-11}} {\mathrm{TeV}\,\mathrm{cm}^2\,\mathrm{s}} \frac{E}{500\,
\mathrm{GeV}}^{-2.95\pm{0.12_\mathrm{stat}}\pm{0.2_\mathrm{syst}}}$$ with a reduced $\chi^2$/dof of 8.56/5, indicating a reasonable description of the data by the fit. For comparison, the Whipple measurement of the 1ES2344+514 spectrum during the flare of 1995 December 20 [@Schroedter] and the Crab Nebula spectrum [@Crab_MAGIC] as obtained with MAGIC are also shown in Fig. \[fig:spectrum\]. Note that the integral flux $F(E>970\,\mathrm{GeV})=(0.82\pm0.09)
\times10^{-12}\,\mathrm{cm}^{-2}\,\mathrm{s}^{-1}$ is in very good agreement with the HEGRA measurements from 1998 to 2002 [@Tluczykont].

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   Mean energy   Bin Width           Flux           Stat. Error             
   $E$ \[GeV\]    \[GeV\]                                                   
       