tokens: line properties.) In our initial line list, we use the former model, adopting the tuned of −0.224 from DM12 . This blended feature is addressed more fully in the next section. We use this initial line list to generate synthetic spectra of the benchmark stars without any Be to compare to the observed spectra, as shown in Figure 3 . The solar spectrum clearly requires the inclusion of Be absorption to fit the observed spectrum at the location of both Be ii lines. In the modeled solar spectrum, the contentious Mn i line at λ 3131.037 Å is clearly visible in the blue wing of the Be line at λ 3131.065 Å. The Mn i line is stronger in the red giant spectra and is well fit with the larger adopted from DM12 . All three benchmark observations show excess absorption predicted by the models, especially below λ 3130.0 Å. Most concerning is that the Arcturus model is a poor fit to the spectrum in the contentious blue wing of the λ 3131.065 Å Be line. Some tuning of the gf -values is therefore required. 4.2. Tuning the Line List The poor fit seen at λ ≲ 3129.6 Å has little effect on the Be abundance analysis, but we did trace the problem to two Fe lines: λ 3129.102 Å (Peterson Kurucz 2015 ) and λ 3129.619 (VALD K14). Removing these lines (which we achieved by changing the by the arbitrarily large factor of −10) produces a much better fit to the spectrum. The focus of the remainder of astrophysical tuning is on a narrow wavelength region around the redder Be ii line, which is the more isolated of the two lines. Despite the relative isolation, there are still significant blends including the contentious Mn i noted earlier as well as a contribution in the red wing of the line by Zr i at λ 3131.109 Å. In the solar spectrum, this line is weak (∼1.5 mÅ equivalent width), but the equivalent width is at least an order of magnitude larger in red giant stars. Furthermore, Figure 3 shows that a nearby Cr i line is poorly fit in the solar spectrum and is nearby enough to potentially affect the neighboring Be blend. The synthesized Cr i line at λ 3131.212 Å is too weak in the spectra of all three benchmark stars. Its was increased by 0.60 dex in order to match the observed solar spectrum. Figure 3. Comparison of synthetic spectra generated with the newly compiled line list (solid lines) compared to observations (dotted lines), assuming no Be in the stellar atmospheres. The dashed vertical lines show the location of the Be ii lines, and the dotted–dashed vertical line marks the Mn i line at λ 3131.037 Å, using the tuned of −0.224 from DM12 . The solar spectrum (top, archival Subaru spectrum of Vesta) is clearly not well fit when Be is absent from the model. The spectrum of Pollux (middle) shows a generally good fit at wavelengths above ∼3130.5 Å, whereas the model for Arcturus (bottom) has conspicuous missing absorption just blue ward of the λ 3131.065 Å Be ii line. As we considered additional changes to the line list in the blended Be feature, we generated spectra
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