High-resolution Laboratory Measurements of Coronal Lines near the Fe ix Line at 171 Å

We present high-resolution laboratory measurements in the spectral region between 165 and 175 A that focus on the emission from various ions of C, O, F, Ne, S, Ar, Fe, and Ni. This wavelength region is centered on the λ171 Fe ix channel of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory, and we place special emphasis on the weaker emission lines of Fe ix predicted in this region. In general, our measurements show a multitude of weak lines missing in the current databases, where the emission lines of Ni are probably most in need of further identification and reclassification. We also find that the wavelengths of some of the known lines need updating. Using the multi-reference Moller–Plesset method for wavelength predictions and collisional-radiative modeling of the line intensities, we have made tentative assignments of more than a dozen lines to the spectrum of Fe ix, some of which have formerly been identified as Fe vii, Fe xiv, or Fe xvi lines. Several Fe features remain unassigned, although they appear to be either Fe vii or Fe x lines. Further work will be needed to complete and correct the spectral line lists in this wavelength region.