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Fig. 2.


Dynamical spectra of selected circumstellar and photospheric lines (as labeled) of the HR 6819 system, phased with the orbital period (see Table 2) of the inner binary. The individual line profiles are overplotted at the top of each panel; the dashed horizontal lines identify the range of the color-coding in the dynamical spectra. The Hα panel was constructed with data set B alone (see Table 1) to minimize the effect of the long-term disk variability of the Be star on the appearance of the emission. The basically invariant RV of the Be star is clearly visible in the peaks of its circumstellar emission lines (e.g., Fe II) as well as in the broad, weak absorption bases of predominantly photospheric lines such as He I. The cuts in the Hδ panels were chosen to highlight that at the 5% level (one tick mark in the upper panel) no feature moves in antiphase with respect to the line core. See Fig. C.2 for additional spectral lines.

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