  The Extreme-ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft
observed flare footpoint regions coincident with a surge for a M3.7 flare
observed on 25 September 2011 at N12 E33 in active region 11302. The flare was
observed in spectral lines of O VI, Fe X, Fe XII, Fe XIV, Fe XV, Fe XVI, Fe
XVII, Fe XXIII and Fe XXIV. The EIS observations were made coincident with hard
X-ray bursts observed by the Reuven Ramaty High Energy Solar Spectroscopic
Imager (RHESSI). Overlays of the RHESSI images on the EIS raster images at
different wavelengths show a spatial coincidence of features in the RHESSI
images with the EIS upflow and downflow regions, as well as loop-top or
near-loop-top regions. A complex array of phenomena was observed including
multiple evaporation regions and the surge, which was also observed by the
Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) telescopes.
The slit of the EIS spectrometer covered several flare footpoint regions from
which evaporative upflows in Fe XXIII and Fe XXIV lines were observed with
Doppler speeds greater than 500 km s$^{-1}$. For ions such as Fe XV both
evaporative outflows (~200 km s$^{-1}$) and downflows (~30-50 km s$^{-1}$) were
observed. Non-thermal motions from 120 to 300 km s$^{-1}$ were measured in
flare lines. In the surge, Doppler speeds are found from about 0 to over 250 km
s$^{-1}$ in lines from ions such as Fe XIV. The non-thermal motions could be
due to multiple sources slightly Doppler-shifted from each other or turbulence
in the evaporating plasma. We estimate the energetics of the hard X-ray burst
and obtain a total flare energy in accelerated electrons of
$\geq7\times10^{28}$ ergs. This is a lower limit because only an upper limit
can be determined for the low energy cutoff to the electron spectrum. We find
that detailed modeling of this event would require a multi-threaded model due
to its complexity.
