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Fig. 8


Hertzsprung-Russell diagram showing the positions of our target stars (full dots, in blue), together with Yonsei-Yale (Y2) evolutionary tracks for solar abundance stars with initial masses of 1, 1.5, and 3 M. For FG Ser, ER Del, and AG Peg, we have only lower limits for the bolometric magnitude. The range for V1261 Ori is indicated with the red dashed line. For HD 190658, we indicate in magenta (open square) the value using the published and seemingly incorrect parallax (7.92 mas) and in green (full triangle) the value with our newly derived parallax.

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