Example galaxy with Bayes factor > 100. Top: observed spectrum (blue line) and the two models, one with high f_esc (solid orange line) and one with f_esc = 0 (dashed magenta line). The shaded gray region represents the masked area. A clear difference between the two models can be seen in the β_UV part of the spectrum, where the high f_esc solution fits the data much better than the other solution. Middle: difference between two models highlighting the difference in the β_UV slope and to some extent in the emission-line strengths. Bottom: Comparison of SFH for the two models. The models are extremely different, as reproducing the weak lines and steep β_UV slope without f_esc is only possible with a recent quenching of star formation. This indicates a degeneracy between SFH and f_esc, which is discussed further in Section 7.