Notes. The second through sixth columns show the distances, periods, characteristic ages, spindown powers in units of 10³³ erg s⁻¹, and transverse velocities of the pulsars with detected FUV BSNe. The eighth and ninth columns show the observed (absorbed) fluxes from the entire BSNe in Hα and FUV (in 1250–1850 Å range), in units of 10⁻¹⁴ erg cm⁻² s⁻¹. We recalculated the J0437 and J2124 BSNe FUV fluxes for the 1250–1850 Å range, using the results obtained by Rangelov et al. (2016, 2017). The tenth column shows the corresponding FUV luminosities in units of 10²⁹ erg s⁻¹. The angular distances between the pulsar and the forward bow shock apex and the corresponding projected distances in units of 10¹⁵ cm are in the eleventh and twelfth columns, while the thirteenth column shows the ratio of count rates in the F125LP to F140LP filters. The FUV fluxes were estimated assuming PL BSN spectra. The two J0437 BSN FUV flux values correspond to different background choices (see Rangelov et al. 2016). The lower limits in square brackets for J1741 were obtained assuming a line-dominated spectrum. The FUV fluxes and luminosities for the entire J0437 and J2124 BSNe were crudely estimated using the apex FUV fluxes from Rangelov et al. (2016, 2017) and assuming similar FUV and Hα brightness distributions for these BSNe.