tokens: optically thin, and uniformly expanding shells as the source of emission in the line wings, since they produce a top-hat line profile without individual emission peaks (e.g., Zuckerman 1987 , pp. 185–209; Cid Fernandes Terlevich 1994 ; Tenorio-Tagle et al. 1996 ; and also the Appendix ). However, the two-hump emission can be caused by a non-spherically symmetric shell or a shell having internal absorption (the other alternatives are analyzed and discarded in Section 5.2 ). Even though the observed amplitudes are similar, the blue component of each pair tends to be larger than the red component. Figure 9 shows the ratio between the areas of the red and blue components, and in all but one case, this ratio is one or smaller, considering error bars. Moreover, if one of the components is missing, it tends to be the red one. These two facts suggest a dusty expanding shell model, where the receding cap of the shell is obscured by the approaching cap (see the Appendix and Figure 17 ). These issues are discussed in detail in Section 5.2 . The color code employed in Figures 9 – 15 assigns a color to each galaxy, and then the different symbols of the same color correspond to the various pairs of secondary components in that galaxy. Figure 9. Area ratio between the blue and red emission of paired components vs. mean strength of the secondary components relative to the central component, i.e., area ratio vs. ε . Each point corresponds to one pair in one of the galaxies, as indicated in the inset—each galaxy has a color, and different symbols with the same color correspond to different weak components of the same galaxy. When only one component exists, it tends to be the blue one (they are marked with an asterisk in the inset). We show unpaired components as having an area ratio equal to zero. Except for ML32, the ratio is consistent with one or smaller. There is no obvious trend in the observed scatter plot. Using the equations in Section 3.3 , we have estimated the mass, mass loss rate, and kinetic energy associated with all the weak components in the H α wings (Section 3.2 , Figure 3 ). The mean values, as well as the errors, are given in Table 4 . The velocities and the ratio between the secondary components and the central component, ε , are provided directly by the multi-Gaussian fit described in Section 3.2 . In the case of paired components, the velocity is the mean of the absolute values of the two velocities, and ε is the total ε of the pair. The estimates also depend on the temperature and electron density of the emitting plasma, as well as on the relative thickness of the shell, , and the filling factor, f . Table 4 Parameters for the Weak Components in the H α Wings a Notes. a The errors in this table represent the standard deviation across the starburst (for velocity, ε , and area ratio) or errors for the value obtained from the mean H α line of the starburst (for the rest). b The number added to the galaxy name identifies each of the pairs of
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