  We present the results from a multiwavelength campaign on the TeV blazar 1ES
1959+650, performed in May, 2006. Data from the optical, UV, soft- and
hard-X-ray and very high energy (VHE) gamma-ray (E > 100 GeV) bands were
obtained with the SUZAKU and SWIFT satellites, with the MAGIC telescope and
other ground based facilities. The source spectral energy distribution (SED),
derived from SUZAKU and MAGIC observations at the end of May 2006, shows the
usual double hump shape, with the synchrotron peak at a higher flux level than
the Compton peak. With respect to historical values, during our campaign the
source exhibited a relatively high state in X-rays and optical, while in the
VHE band it was at one of the lowest level so far recorded. We also monitored
the source for flux-spectral variability on a time window of 10 days in the
optical-UV and X-ray bands and 7 days in the VHE band. The source varies more
in the X-ray, than in the optical band, with the 2-10 keV X-ray flux varying by
a factor of ~2. The synchrotron peak is located in the X-ray band and moves to
higher energies as the source gets brighter, with the X-ray fluxes above it
varying more rapidly than the X-ray fluxes at lower energies. The variability
behaviour observed in the X-ray band cannot be produced by emitting regions
varying independently, and suggests instead some sort of ``standing shock''
scenario. The overall SED is well represented by an homogeneous one-zone
synchrotron inverse Compton emission model, from which we derive physical
parameters that are typical of high energy peaked blazars.
