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A Suzaku X-ray observation of NGC 4051 taken during 2005 Nov reveals lineemission at 5.44 keV in the rest-frame of the galaxy which does not have anobvious origin in known rest-frame atomic transitions. The improvement to thefit statistic when this line is accounted for establishes its reality at >99.9%confidence: we have also verified that the line is detected in the three XISunits independently. Comparison between the data and Monte Carlo simulationsshows that the probability of the line being a statistical fluctuation is p <3.3 x 10^-4. Consideration of three independent line detections in Suzaku datataken at different epochs yields a probability p< 3 x 10^-11 and thusconclusively demonstrates that it cannot be a statistical fluctuation in thedata. The new line and a strong component of Fe Ka emission from neutralmaterial are prominent when the source flux is low, during 2005. Spectra from2008 show evidence for a line consistent with having the same flux and energyas that observed during 2005, but inconsistent with having a constantequivalent width against the observed continuum. The stability of the line fluxand energy suggests that it may not arise in transient hotspots, as has beensuggested for similar lines in other sources, but could arise from a speciallocation in the reprocessor, such as the inner edge of the accretion disk.Alternatively, the line energy may be explained by spallation of Fe into Cr, asdiscussed in a companion paper.

Significant X-ray Line Emission in the 5-6 keV band of NGC 4051