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We present the results from a multiwavelength campaign on the TeV blazar 1ES1959+650, performed in May, 2006. Data from the optical, UV, soft- andhard-X-ray and very high energy (VHE) gamma-ray (E > 100 GeV) bands wereobtained with the SUZAKU and SWIFT satellites, with the MAGIC telescope andother ground based facilities. The source spectral energy distribution (SED),derived from SUZAKU and MAGIC observations at the end of May 2006, shows theusual double hump shape, with the synchrotron peak at a higher flux level thanthe Compton peak. With respect to historical values, during our campaign thesource exhibited a relatively high state in X-rays and optical, while in theVHE band it was at one of the lowest level so far recorded. We also monitoredthe source for flux-spectral variability on a time window of 10 days in theoptical-UV and X-ray bands and 7 days in the VHE band. The source varies morein the X-ray, than in the optical band, with the 2-10 keV X-ray flux varying bya factor of ~2. The synchrotron peak is located in the X-ray band and moves tohigher energies as the source gets brighter, with the X-ray fluxes above itvarying more rapidly than the X-ray fluxes at lower energies. The variabilitybehaviour observed in the X-ray band cannot be produced by emitting regionsvarying independently, and suggests instead some sort of ``standing shock''scenario. The overall SED is well represented by an homogeneous one-zonesynchrotron inverse Compton emission model, from which we derive physicalparameters that are typical of high energy peaked blazars.

Simultaneous multiwavelength observations of the blazar 1ES1959+650 at a low TeV flux