We present a study of a recurring jet observed on October 31 , 2011 by SDO/AIA , Hinode/XRT and Hinode/EIS .
We discuss the physical parameters of the jet such as density , differential emission measure , peak temperature , velocity and filling factor obtained using imaging and spectroscopic observations .
A differential emission measure ( DEM ) analysis was performed at the region of the jet-spire and the footpoint using EIS observations and also by combining AIA and XRT observations .
The DEM curves were used to create synthetic spectra with the CHIANTI atomic database .
The plasma along the line-of-sight in the jet-spire and jet-footpoint was found to be peak at 2.0 MK .
We calculated electron densities using the Fe XII ( \lambda 186/ \lambda 195 ) line ratio in the region of the spire ( N _ { \textrm { e } } = 7.6 \times 10 ^ { 10 } cm ^ { -3 } ) and the footpoint ( 1.1 \times 10 ^ { 11 } cm ^ { -3 } ) .
The plane-of-sky velocity of the jet is found to be 524 km/s .
The resulting EIS DEM values are in good agreement with those obtained from AIA-XRT .
There is no indication of high temperatures , such as emission from Fe XVII ( \lambda 254.87 ) ( log T [ K ] = 6.75 ) seen in the jet-spire .
In case of the jet-footpoint , synthetic spectra predict weak contributions from Ca XVII ( \lambda 192.85 ) and Fe XVII ( \lambda 254.87 ) .
With further investigation , we confirmed emission from the Fe XVIII ( \lambda 93.932 Å ) line in the AIA 94 Å channel in the region of the footpoint .
We also found good agreement between the estimated and predicted Fe XVIII count rates .
A study of the temporal evolution of the jet-footpoint and the presence of high-temperature emission from the Fe XVIII ( log T [ K ] = 6.85 ) line leads us to conclude that the hot component in the jet-footpoint was present initially that the jet had cooled down by the time EIS observed it .