tokens: of the blended line intensities of Fe xiii and Fe xii in the analysis of EIS spectra, we applied the same method to the Fe xvii line complex around λ 204.6 Å in the LHD spectra to unblend the Fe xiii and xii line intensities. The results are summarized in Figure 5 . The time evolution of the electron density for low-temperature LHD peripheral plasmas is plotted in Figure 5 (a), where the electron density ( n e ) is estimated to be log n e (cm −3 ) ∼ 10.5–11.8 after the NBI controls, slightly higher in the later phases of discharge. The estimated electron densities are somewhat lower than those measured by Thomson scattering at t = 4.3 s and t = 4.9 s (see Figure 2 of Murakami et al. 2014 ), but these line intensity ratios of Fe xii and xiii are located in the range that is close to the high-density limit, and the apparent large difference in the absolute n e values derived from Fe xii and Fe xiii does not affect the estimation of the blended Fe xiii/xii line intensities much, and therefore is negliglible in the following analysis results. Figure 5. (a) Electron densities for the LHD plasma plottted against time since the discharge of shot 107,802. The line types are the same as in Figure 4 (b). (b) Reduced Fe xvii line ratios by unblending the contributions of the Fe xii and xiii lines. The horizontal thin dotted line indicates the line intensity ratio averaged at the eight epochs in discharge 107,802. Error bars show photon noise ranges only. We take this contribution of the Fe xiii emissions to the emission line intensity at 204.6 Å into account and plot the Fe xvii λ 204.6/ λ 254.8 ratios against time after the start of discharge in Figure 5 (b). No lines are assumed to be blended in the Fe xvii λ 254.8 line, and a common electron density is assumed for the Fe xii/xiii emitting plasmas. The measured ratio is reduced to 20%–30% as a result of subtracting the Fe xiii line contribution, and the average value (∼1.12) is very close to the theoretically predicted constant vlaue of ∼1.1, although the temporal variation, henceforth, the temperature dependence of the line ratios, could not be completely eliminated in this analysis. The average value at the four epochs ( t = 4.8–5.4 s) is rather close to ∼1.3, when the line complexes at 204.6 Å are the strongest and the electron temperatures are the lowest during the discharge. 4. Discussion and Summary The Fe xvii line intensity ratios obtained from the solar active region in Section 2.3 and the LHD experiment are plotted against electron temperature in Figure 6 , in which the revised sensitivity proposed by Del Zanna ( 2013 ) is adopted for the EIS radiometric calibration. The LHD experimental results clearly show that the Fe xvii line branching ratio of λ 204.6/ λ 254.8 is close to the theoretical value of ∼1.1, which means that the revised in-orbit EIS sensitivity calibration (Del Zanna 2013 ; Warren et al. 2014 ) makes the solar data consistent with the laboratory data. The apparent
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