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Abstract

Of the two solar lines, K I D₁ and D₂, almost all attention so far has been devoted to the D₁ line, as D₂ is severely affected by an O₂ atmospheric band. This, however, makes the latter appealing for balloon and space observations from above (most of) the Earth’s atmosphere. We estimate the residual effect of the O₂ band on the K I D₂ line at altitudes typical for stratospheric balloons. Our aim is to study the feasibility of observing the 770 nm window. Specifically, this paper serves as a preparation for the third flight of the Sunrise balloon-borne observatory. The results indicate that the absorption by O₂ is still present, albeit much weaker, at the expected balloon altitude. We applied the obtained O₂ transmittance to K I D₂ synthetic polarimetric spectra and found that in the absence of line-of-sight motions, the residual O₂ has a negligible effect on the K I D₂ line. On the other hand, for Doppler-shifted K I D₂ data, the residual O₂ might alter the shape of the Stokes profiles. However, the residual O₂ absorption is sufficiently weak at stratospheric levels that it can be divided out if appropriate measurements are made, something that is impossible at ground level. Therefore, for the first time with Sunrise III, we will be able to perform polarimetric observations of the K I D₂ line and, consequently, we will have improved access to the thermodynamics and magnetic properties of the upper photosphere from observations of the K I lines.