  Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron
stars with ultra strong magnetic field of $10^{14}$-- $10^{15}$ G. Their energy
spectra below $\sim$10 keV are modeled well by two components consisting of a
blackbody (BB) ($\sim$0.4 keV) and rather steep power-law (POW) function
(photon index $\sim$2-4). Kuiper et al.(2004) discovered hard X-ray component
above $\sim$10 keV from some AXPs. Here, we present the Suzaku observation of
the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this
observation, we could analyze the spectrum from 0.4 to 50 keV at the same time.
Then, we could test whether the spectral model above was valid or not in this
wide energy range. We found that there were residual in the spectral fits when
fit by the model of BB + POW. Fits were improved by adding another BB or POW
component. But the meaning of each component became ambiguous in the
phase-resolved spectroscopy. Alternatively we found that NPEX model fit well
for both phase-averaged spectrum and phase-resolved spectra. In this case, the
photon indices were constant during all phase, and spectral variation seemed to
be very clear. This fact suggests somewhat fundamental meaning for the emission
from magnetars.
