of this AGN. An SSC model is used to describe the wide-range spectral energy distribution (SED).

Observations
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The observations were performed between 2005 August 3 and 2005 September 29, and between 2005 November 11 and 2006 January 1, using the MAGIC Telescope on the Canary island of La Palma ($28.8^\circ$N, $17.8^\circ$W, 2200 m above sea level), from where 1ES2344+514 can be observed at zenith distances above $24^\circ$. The essential parameters of the currently largest air Cherenkov telescope are a 17 m ø segmented mirror of parabolic shape, an $f/D$ of 1.05 and a hexagonally shaped camera with a field of view (FOV) of $\approx3.5^\circ$ mean diameter. The camera comprises 576 pixels composed of hemispherical, six dynode photomultipliers augmented in sensitivity by a diffuse lacquer doped with a wavelength shifter [@Paneque] and by so-called light catchers. In separate measurements a total gain of 2 has been determined. 180 pixels of $0.2^\circ$ ø surround the inner section of the camera, which consists of 394 pixels of $0.1^\circ$ ø ($= 2.2^\circ$ ø FOV). The trigger is formed by a coincidence of $\geq 4$ neighboring pixels. The overall Cherenkov photon ($300-650$ nm) to photoelectron conversion ratio is $0.15\pm0.02$. The point spread function (PSF) 