Comparison of the final L_X–a-distributions for the Owen_XX models using the photoevaporation profile by O12. The different rows show the outcomes of the population synthesis models using different insertion locations of the planets (5 au, 10 au, 20 au and random insertion locations). Colours in the left column correspond to the formation time of the planet with respect to the disc clearing time due to photoevaporation. In the right column, colours reflect the initial planetary mass. The black lines highlight the different regimes, in which the final planet parking location is set by different effects. These are discussed in detail in Sect. 4.1. The red lines in the right panels correspond to the XLFs as shown in Fig. 3. Additionally, the data points were weighted linearly following the XLF in Taurus so that their size reflects the observing probability at a given L_X. This step was performed in order to emphasise which regions in L_X-parameter space are strongly over-crowded due to the linear sampling of_X in our model.