Fig. 8
Hα line profiles of two known SySts, AS 245 and BX Mon, and two candidate SySts, M 2−9 and M 1−91. The data were obtained from the San Pedro Mártir observatory (Akras et al., in prep.). The x-axis represents the expansion velocities, where arbitrarily it has been given a zero velocity to the absorption dips for direct comparison.
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