used here, as the radio emission is thought to arise from a larger volume in the jet than the VHE $\gamma$-ray emission and as self-absorption effects are not accounted for.

Two [*BeppoSAX*]{} data sets are shown: one was obtained simultaneously with Whipple observations on 1996 December 5. The second set was taken during a quiescent period of 1ES2344+514, and represents a rather low X-ray emission state of the object, although it might not necessarily correspond to its state during the MAGIC measurements. It should be emphasized that most of the data points shown in the SED were not measured simultaneously, which makes the SED modeling very difficult. The input parameters of the homogeneous SSC model are the radius of the spherically assumed emission region $R$, the Doppler factor $\delta$, the magnetic field strength $B$ in the acceleration region, the density $\rho$ of the electrons responsible for the $\gamma$-ray emission as well as two spectral slopes and a spectral cutoff of the electron spectrum. The size of the emission region $R$ was chosen such that it can account for day-scale variability along with the Doppler factor $\delta$ chosen, $R \leq \delta_{-1} \times t_{\mathrm{d}} \times
2.48 \times 10^{16} \mathrm{cm}$ with $\delta_{-1}=\delta / 