Energy spectrum of EXO 2030+375 obtained with the XIS, PIN, and GSO detectors of the Suzaku observation at the peak of the type I outburst, along with the best-fit model comprising a partially absorbed power law with a high-energy cutoff continuum model with a partially ionized absorber. The emission lines (as given in Table 1) detected in the pulsar spectrum are represented by Gaussian functions in the figure. The contributions of the residuals to the χ ² for each energy bin for the best-fit model are shown in the bottom panel.