Top: spin period and DM of pulsars that have been discovered (black dots) and redetected (red circles) in the LOTAAS survey. The size of the circles for the redetected pulsars denotes their flux density. Also plotted as thin grey points are known pulsars from the ATNF pulsar catalogue (excluding pulsars in globular clusters). The solid lines denote the sensitivity limits (in mJy) when taking into account smearing due to dispersion (black), as well as scattering, using the Bhat et al. (2004) (green) and Geyer et al. (2017) (blue) scattering relations. Bottom: cumulative spin period distributions for the pulsars discovered (black) and redetected (red) in the LOTAAS survey. These can be compared to the spin period distribution of pulsars from the ATNF catalogue (dark grey, again excluding pulsars in globular clusters), and when keeping pulsars with P >  0.02 s and DM <  200 pc cm⁻³ (light grey). The latter distribution can represent the distribution of pulsars that have been redetected in the LOTAAS survey. However, the LOTAAS discoveries tend to have longer spin periods, on average.