\begin{table}%t4 \par \caption{\label{tab:measured_lambda}List of measured wavelengths.} %\centerline {\footnotesize\begin{tabular}[c]{@{}lcl@{}} \hline\hline \noalign{\smallskip} $\lambda_{\rm meas}$(\AA) & $\lambda_{\rm lit}$(\AA) & ID \\ \noalign{\smallskip}\hline\noalign{\smallskip} %inserts single line 185.214 & 185.213 & Fe VIII (bl oc Ni XVI 185.23) \\ 186.607 & 186.601 & Fe VIII (bl oc Ca XIV 186.61) \\ 187.243 & 187.237 & Fe VIII \\ 191.585 & 191.570 & Mn IX \\ 192.000 & 192.004 & ? Fe VIII (bl oc Fe XI Fe XXIV) \\ 192.087 & -- & u (VIII-IX) \\ 193.972 & 193.967 & Fe VIII \\ 194.658 & 194.662 & Fe VIII \\ %194.778 & - & u (IX) \\ 195.969 & ? 195.972 & Fe VIII (bl) \\ 196.649 & 196.650 & Fe VIII (bl oc Fe XII) \\ 197.364 & 197.362 & Fe VIII (bl) \\ 204.704 & -- & Fe VIII (bl oc Fe XVII) \\ % \ion{Fe}{xvii} 205.04 & 205.040 & Cr VIII \\ 205.708 & 205.720 & Cr VIII \\ 206.761 & -- & Fe VII \\ 207.124 & -- & Fe VIII \\ 207.203 & -- & u (VI?) \\ 207.725 & -- & u (VI?) \\ \noalign{\smallskip} 217.71 & 217.691 & Fe VIII \\ 218.57 & 218.564 & Fe VIII \\ 222.19 & -- & Fe VIII \\ 224.28 & 224.305 & Fe VIII \\ 225.40 & -- & Fe VIII \\ 227.29 & -- & Fe VIII \\ 231.03 & 231.097 & Fe VIII \\ 231.81 & 231.884 & Fe VIII \\ \noalign{\smallskip} 246.011 & 246.004 & Si VI (bl) \\ 249.135 & 249.124 & Si VI (bl oc Ni XVII) \\ 253.520 & -- & ? Fe VII \\ 253.956 & -- & Fe VIII (bl oc S X) \\ 254.059 & -- & Fe VII \\ 255.110 & -- & Fe VIII (bl oc S X, Fe XXIV) \\ 255.346 & -- & Fe VIII \\ 255.684 & -- & Fe VIII \\ 268.996 & 268.991 & Mg VI \\ 270.401 & 270.391 & Mg VI \\ 272.661 & 272.639 & Si VII (bl) \\ 275.370 & 275.353 & Si VII \\ 275.686 & 275.667 & Si VII (bl) \\ 276.145 & 276.153 & Mg VII \\ % ?? 280.732 & 280.737 & Mg VII \\ \noalign{\smallskip} \hline %inserts single line \end{tabular}} \par \smallskip Note: $\lambda_{\rm meas}$(\AA) are the measured wavelengths for \ion{Fe}{viii}~lines and a selection of lines from ions formed at similar temperatures. Results are from the Hinode EIS spectrum of the ``foreground-subtracted'' Sunspot loop leg and from the laboratory spectrum. Uncertainties are estimated to be about 0.01~\AA. In the second column wavelengths from the literature ($\lambda_{\rm lit}$) are listed. A few of the main lines which are potentially blending (bl) are also noted. Some of the unidentified (u) TR lines are listed, together with the Fe ionization stage which more closely resembles their morphology. oc: blended in other plasma conditions. \end{table}