Erratum to: Solar Phys. (2012) 280:425–434 DOI 10.1007/s11207-012-9986-8

A mistake in our program has lead to the erroneous calculation of the spicule DEM. The figures and calculations given in the paper have changed. The corrected versions are presented here. We apologize for this late clarification.

Figure 2 from the paper should be changed to the one below.

The values for radiance given in Table 1 have been corrected.

The modified version of Figure 4 is given below.

The calculations we did in Section 4 are modified and should read as:

From the graphs in Figure 4 we were able to numerically integrate the values to obtain what percent of plasma seen in the 171 Å filter is above million degrees. We find that in the case of spicule or prominence observations the contribution is only 1.3 % and 2.5 %, respectively, whereas for the quiet Sun it is a little over 23 %.

However, our main conclusion still remains the same. During spicule observations the emission in the Fe ix 171 Å filter comes from plasma at transition region temperatures rather than coronal.

Figure 2
figure 1

The DEM for off-limb data (where spicules are most easily identified) is calculated for different abundances as indicated in the legend using CHIANTI 7.1.

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Figure 4
figure 2

The contribution function G(N,T) for Fe ix 171.07 Å (bold, solid line) is plotted along with the normalised product G(N,T)×DEM(T) for three different DEMs (a) off-limb, (b) prominence and (c) quiet Sun and for different solar abundances as indicated in the legend.

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Table 1 Details of the SUMER spectral lines used for the construction of the DEM.
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