Chromosphere break as a function of chromospheric filling factor for models that match the ranges of log(﹩{{L}_{{\rm H}\alpha }}/{{L}_{{\rm bol}}}﹩) for each ﹩{{T}_{{\rm eff}}}﹩/spectral type shown in Figure 12. For each ﹩{{T}_{{\rm eff}}}﹩, the large circles are values that match the inner quartile range of observed values, while the smaller circles show matches with the entire range of values. Circles are slightly offset from their exact values for clarity. The left panel corresponds to the left panel of Figure 12, illustrating the models that best match the values adopted from the Hα emission data. The right panel corresponds to the right panel of Figure 12, showing the models that best match the “test” values adopted to examine the effect of the biases (e.g., inclusion of serendipitous flare emission from M4 dwarfs and the Hα detection limit in SDSS) described further in Section 7.