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Fig. 9

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The peak velocity (half the peak-to-peak velocity) of all double-peaked emission lines in B243, B268, and B275 is plotted against their V/R ratios. The data points represent the line properties in one epoch of each star. The emission lines in a single epoch of a star have different V/R ratios and peak velocities. For B243 and B275, the lower excitation lines form at relatively lower velocities, hence at more slowly rotating parts of the disk, and their V/R ratios are relatively lower, meaning that their red peak is stronger than the blue, than measured for the higher excitation lines. For both stars, this results in a trend of a higher V/R ratio with a higher disk velocity. The displayed epochs are for B243: 2012-07-06, B268: 2019-05-31, and B275: 2019-07-09.

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