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In this work we investigate the thermal structure of an off-limb activeregion in various non-flaring areas, as it provides key information on the waythese structures are heated. In particular, we concentrate in the very hotcomponent (>3 MK) as it is a crucial element to discriminate between differentheating mechanisms. We present an analysis using Fe and Ca emission lines fromboth SOHO/SUMER and HINODE/EIS. A dataset covering all ionization stages fromFe X to Fe XIX has been used for the thermal analysis (both DEM and EM). Ca XIVis used for the SUMER-EIS radiometric cross-calibration.  We show how the very hot plasma is present and persistent almost everywherein the core of the limb AR. The off-limb AR is clearly structured in Fe XVIII.Almost everywhere, the EM analysis reveals plasma at 10 MK (visible in Fe XIXemission) which is down to 0.1% of EM of the main 3 MK plasma. We estimate thepower law index of the hot tail of the EM to be between -8.5 and -4.4. However,we leave an open question on the possible existence of a small minor peak ataround 10 MK. The absence in some part of the AR of Fe XIX and Fe XXIII lines(which fall into our spectral range) enables us to determine an upper limit onthe EM at such temperatures. Our results include a new Ca XIV 943.59 \AA~atomic model.

Spectroscopy of very hot plasma in non-flaring parts of a solar limb active region: spatial and temporal properties