Stripped stars formed through each of the 3 channels considered, as raw numbers (left) and as a fraction of the total (right). We display the distributions for one of the solar metallicity model runs, although the metallicity distributions in general show similar trends. Common envelope evolution accounts for ∼20% of stripped stars across most mass bins and in total. Stable mass transfer during the Hertzsprung gap is the most common channel for M ≲ 15 M_⊙, and stable mass transfer during the main sequence becomes more common at the very high-mass end. The stripped star masses of those formed through the latter channel may have been slightly overestimated.