Table 1.
Spectral lines and bands.
| Linea/bandb | log T [K] c | ||
|---|---|---|---|
| H I | 1025.728 Å | 4.00 | |
| C III | 977.020 Å | 4.85 | |
| SPICE | S V | 786.468 Å | 5.20 |
| O IV | 787.710 Å | 5.15 | |
| O VI | 1031.912 Å | 5.50 | |
| Ne VIII | 770.409 Å | 5.80 | |
| 304 Å | (He II) | 4.92 | |
| 131 Å | (Fe VIII)d | 5.72 | |
| 171 Å | (Fe IX) | 5.91 | |
| AIA | 193 Å | (Fe XII) | 6.18 |
| 211 Å | (Fe XIV) | 6.27 | |
| 335 Å | (Fe XVI) | 6.40 | |
| 94 Å | (Fe XVIII)d | 6.86 | |
Notes.
For the SPICE emission lines, we list the rest wavelengths from the NIST database (https://dx.doi.org/10.18434/T4W30F).
For the SPICE emission lines, we list the temperature in log T [K] at which the ion fraction peaks in ionization equilibrium, based on CHIANTI. For the AIA bands, we list the peak temperature of the response function based on Peter et al. (2012) (their Fig. 1).
The 131 Å band also receives a contribution at about 10 MK from Fe XXI (Lemen et al. 2012), which is not relevant for the observations of the coronal bright points. On the other hand, the 94 Å band receives a relevant contribution at around 1 MK from Fe X (cf. Table 1 of Martínez-Sykora et al. 2011).
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