  Measuring the relative amount of high-temperature, low-emission-measure
plasma is considered to be a smoking gun observation to constrain the frequency
of plasma heating in coronal structures. Often, narrowband, extreme ultraviolet
images, such as those obtained by the Atmospheric Imaging Assembly (AIA) on the
Solar Dynamics Observatory (SDO), are used to determine the emission measure
(EM) distribution, though the sensitivity to high temperature plasma is
limited. Conversely, the soft X-ray wavelength range offers multiple high
temperature diagnostics, including emission lines of N VII, O VII, O VIII, Fe
XVII, Ne IX, and Mg XI, which can provide tight constraints to the high
temperature plasma in the log T 6.1 to 6.7 range. The Marshall Grazing
Incidence X-ray Spectrometer (MaGIXS), a slitless spectrograph launched on a
NASA sounding rocket on July 30, 2021 resolved an X-ray bright point in
multiple emission lines in the soft X-ray wavelength range. Using coordinated
observations of the same X-ray bright point from SDO/AIA, we compare and
contrast the EM distributions from the EUV image data, the X-ray spectra, as
well as the combined EUV and X-ray dataset. In this paper, we demonstrate that
EM distributions from SDO/AIA data alone can overestimate the amount of high
temperature (log T > 6.4) plasma in the solar corona by a factor of 3 to 15.
Furthermore, we present our effort to cross-calibrate Hinode/XRT response
functions by comparing the observed XRT fluxes with the predicted ones from
combined MaGIXS-1 + AIA EM analysis.
