140 GeV and 5.4 TeV ($\chi^2_{\mathrm{dof}} = 0.68/5$). The spectrum shows a tendency to flatten towards low energies. A fit with a logarithmic curvature term, which corresponds to a parabolic law in a $\log(E^2 \mathrm{d}N/\mathrm{d}E)$ vs. $\log
E$ representation (power law index $\alpha \rightarrow a + 2b \log
(E/E_a)$; Massaro et al. 2004), shows a clear curvature and enables locating the peak at $E_{\rm peak} = E_a \cdot
10^{(2-a)/(2b)}=(202\pm174)$ GeV. The peak is obviously badly determined as the turnover of the spectrum, presumably around $200$ GeV, is not observed unambiguously.

![Measured and intrinsic differential photon spectrum of 1ES2344+514. Simple power law fits are given by the dot-dashed and dashed lines, while the fit with a logarithmic curvature term is given by the dotted curve.[]{data-label="fig:spectrumdeabs"}](f6.eps){width="\linewidth"}

Spectral Energy Distribution
----------------------------

![image](f7.eps){width="\linewidth"}

The spectral energy distribution for 1ES2344+514 is shown in Fig. \[fig:wsed\]. Apart from the VHE $\gamma$-ray observations by MAGIC, Whipple, and HEGRA, the X-ray measurements performed by [*Einstein*]{}, [*ROSAT*]{}, and [*BeppoSAX*]{} and an upper limit from [*EGRET*]{} are the most relevant measurements for modeling the SED. The figure also includes optical and radio measurements. The latter however cannot be described by the homogeneous one-zone SSC model provided by @Krawczynski1es1959-2004 that was 