  We study the spatial distribution and evolution of the slope of the Emission
Measure between 1 and 3~MK in the core active region NOAA~11193, first when it
appeared near the central meridian and then again when it re-appeared after a
solar rotation. We use observations recorded by the Extreme-ultraviolet Imaging
Spectrometer (EIS) aboard Hinode, with a new radiometric calibration. We also
use observations from the Atmospheric Imaging Assembly (AIA) aboard Solar
Dynamics Observatory (SDO). We present the first spatially resolved maps of the
EM slope in the 1--3~MK range within the core of the AR using several methods,
both approximate and from the Differential Emission Measure (DEM). A
significant variation of the slope is found at different spatial locations
within the active region. We selected two regions that were not affected too
much by any line-of-sight lower temperature emission. We found that the EM had
a power law of the form EM~$\propto T^{b}$, with b = 4.4$\pm0.4$, and
4.6$\pm0.4$, during the first and second appearance of the active region,
respectively. During the second rotation, line-of-sight effects become more
important, although difficult to estimate. We found that the use of the ground
calibration for Hinode/EIS and the approximate method to derive the Emission
Measure, used in previous publications, produce an underestimation of the
slopes. The EM distribution in active region cores is generally found to be
consistent with high frequency heating, and stays more or less the same during
the evolution of the active region.
