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