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One of the key processes associated with the "standard" flare model ischromospheric evaporation, a process where plasma heated to high temperaturesby energy deposition at the flare footpoints is driven upwards into the corona.Despite several decades of study, a number of open questions remain, includingthe relationship between plasma produced during this process and observationsof earlier "superhot" plasma. Hinode/EIS has a wide slot often used as a flaretrigger in the He II emission line band. Once the intensity passes a thresholdlevel, the study switches to one focussed on the flaring region. However, whenthe intensity is not high enough to reach the flare trigger threshold, thesedatasets are available during the entire flare period and provide high-cadencespectroscopic observations over a large field of view. We use one-minutecadence data from two such studies of a C4.7 flare and a C1.6 flare to probethe relationship between hot Fe XXIV plasma and plasmas observed by RHESSI andXRT to track where the emission comes from, and when it begins. Although thespatial and spectral information are merged in the wide-slot data, it is stillpossible to extract when the hot plasma appears using the Fe XXIV spectralimage. It is also possible to derive spectrally pure Fe XXIV light curves fromthe EIS data, and compare them with those derived from hard X-rays, enabling afull exploration of the evolution of hot emission. The Fe XXIV emission peaksjust after the peak in the hard X-ray lightcurve; consistent with an origin inthe evaporation of heated plasma following the transfer of energy to the loweratmosphere. A peak was also found for the C4.7 flare in the RHESSI peaktemperature, which occurred before the hard X-rays peaked. This suggests thatthe first peak in hot-plasma emission is likely directly related to theenergy-release process.

Locating Hot Plasma in Small Flares using Spectroscopic Overlappogram Data from the Hinode {\it EUV} Imaging Spectrometer