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. Author manuscript; available in PMC: 2017 Jun 2.
Published in final edited form as: Astrophys J Suppl Ser. 2017 Jan 20;228(1):10. doi: 10.3847/1538-4365/228/1/10

Figure 2.

Figure 2

Relative strengths STR of Cr II lines vs. line wavelength. This figure is constructed in the same manner as Figure 5 of Lawler et al. (2015). The vertical blue line indicates the 3000 Å atmospheric cutoff, and the horizontal blue line is placed where the STR values approach the practical weak-line limit in the photospheric spectrum (reduced widths log(RW ) = −6) for abundance analysis. The black points include all 183 transitions with laboratory data reported here, and those points encircled in red indicate those lines used in our solar abundance determination.