We report about very high energy ( VHE ) \gamma -ray observations of the Crab Nebula with the MAGIC telescope .
The \gamma -ray flux from the nebula was measured between 60 GeV and 9 TeV .
The energy spectrum can be described by a curved power law { \mathrm { d } F } / { \mathrm { d } E } = f _ { 0 } \left ( E / 300 \mathrm { GeV } \right ) ^ { \left [ a + b% \log _ { 10 } \left ( E / 300 \mathrm { GeV } \right ) \right ] } with a flux normalization f _ { 0 } of ( 6.0 \pm 0.2 _ { \mathrm { stat } } ) \times 10 ^ { -10 } cm ^ { -2 } s ^ { -1 } TeV ^ { -1 } , a = -2.31 \pm 0.06 _ { \mathrm { stat } } and b = -0.26 \pm 0.07 _ { \mathrm { stat } } .
The peak in the spectral energy distribution is estimated at 77 \pm 35 GeV .
Within the observation time and the experimental resolution of the telescope , the \gamma -ray emission is steady and pointlike .
The emission ’ s center of gravity coincides with the position of the pulsar .
Pulsed \gamma -ray emission from the pulsar could not be detected .
We constrain the cutoff energy of the pulsed spectrum to be less than 27 GeV , assuming that the differential energy spectrum has an exponential cutoff .
For a super-exponential shape , the cutoff energy can be as high as 60 GeV .