Host star effective temperatures of the planets with metastable helium observations in Fig. 5 separated by the accuracy of the model predictions. In this figure, we adopt a relatively strict factor of two when classifying a model as accurate. So, the red histogram includes the planets for which the model helium EW is more than a factor two higher than the observed EW (i.e., both detections and upper limits toward the bottom-right part of Fig. 5). The blue histogram includes the planets with helium detections that are accurately predicted by our model within a factor two. The green histogram includes the planets where a reported upper limit is above half the model value (i.e., upper limits toward the top-left part of Fig. 5; we consider these consistent as well). The yellow histogram includes the planets with detections that are above two times the model EW (i.e., HAT-P-67 b, HAT-P-32 b, and HD 209458 b). We see that our model tends to overestimate the helium signal particularly for planets around M- and K-type stars.