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The Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatoryis a state-of-the-art imager with the potential to do unprecedentedtime-dependent multi-thermal analysis at every pixel on scales short comparedto the radiative and conductive cooling times. Recent results, however, haveidentified missing spectral lines in the CHIANTI atomic physics data base,which is used to construct the instrument response functions. We have donedifferential emission measure analysis using simultaneous AIA and Hinode/EISobservations of six X-ray bright points. Our results not only support theconclusion that CHIANTI is incomplete near 131 angstroms, but more importantly,suggest that the peak temperature of the Fe VIII emissivity/response is likelyto be closer to log T = 5.8 than to the current value of log T = 5.7. Using arevised emissivity/response calculation for Fe VIII, we find that the observedAIA 131-angstrom flux can be underestimated by about 1.25, which is smallerthan previous comparisons.

Atmospheric Imaging Assembly Response Functions: Solving the Fe VIII Problems with Hinode EIS Bright Point Data