The Crab pulsar wind nebula (PWN) is one of the best studied astrophysical objects. Due to itsbrightness at all wavelengths, precise measurements are provided by different kind of instruments,allowing for many discoveries, later seen in other non-thermal sources, and a detailed examinationof its physics. Most of the theoretical models for PWN emission are, in fact, based on Crab nebulameasurements. The Crab nebula shows a broad-band spectrum spanning from radio frequenciesup to VHE gamma rays and consists of two components, one of synchrotron origin and the otherone due to radiative inverse Compton losses, starting at a few GeV. We will report the most precisemeasurements of the inverse Compton component from the Crab Nebula by combining data by theLarge Area Telescope (LAT) on board of the Fermi satellite (1–300 GeV) and by the stereoscopicMAGIC system (>50 GeV). At low energies, the MAGIC results, combined with the Fermi/LATdata, show a flat and broad inverse Compton peak. The overall fit to the data between 1 GeV and30 TeV is well-described by a modified log-parabola function with an exponent of 2.5, and placesthe position of the inverse Compton peak at around 53 GeV. The spectral measurements obtainedby the MAGIC collaboration cover more than three decades in energy, and could help to addressthe still-open question about the maximum energy reached by the parent electron population. Thebroadness of the inverse Compton peak cannot be reproduced by either the constant B-field modelor the MHD flow model. The conclusion, based on earlier data, that simple models (constant B-field, spherical symmetry) can account for the observed spectral shape has to revisited at the lightof the new MAGIC results. On the other hand, the time-dependent 1D spectral model providesa good fit of the new VHE results when considering a 80μG magnetic field. However, it fails tomatch the data when including the morphology of the nebula at lower wavelength.