for VHE $\gamma$-ray emission via inverse Compton (IC) scattering. EGRET did not detect any signal from 1ES2344+514, giving an upper limit of $3.4\times10^{-11}\,\mathrm{erg}\,\mathrm{cm}^{-2}\,\mathrm{s}^{-1}$ at its peak response energy of 300 MeV [@Fichtel]. During the winter of 1995/1996, the Whipple collaboration reported a $5.8\sigma$ excess signal from 1ES2344+514 above 350 GeV from 20.5 hours observation time [@Catanese]. The observed flux was highly variable, with the most significant signal occurring during a flare on 1995 December 20, while all the remaining data combined led to an only marginal ($4\sigma$) excess, i.e. below the canonical detection limit used in ground-based VHE $\gamma$-ray astronomy. The 0.8$-$12.6 TeV differential spectrum measured by the Whipple collaboration during the flare had a power-law index of $-2.54\pm{0.17_\mathrm{stat}}\pm0.07_{\mathrm{syst}}$ [@Schroedter]. One year later another search did not reveal any VHE $\gamma$-ray emission. The HEGRA collaboration also searched for VHE $\gamma$-ray emission above 800 GeV. A deep exposure of 72.5 h indicated a signal at a significance level of $4.4\sigma$ [@Tluczykont].

Here we present MAGIC telescope observations of 1ES2344+514. We briefly discuss the observational technique used and the implemented data analysis procedure, derive a VHE $\gamma$-ray spectrum of the source, and put the results into perspective with other VHE $\gamma$-ray observations 