Notes. Each burst is assigned an ID in the first column. The second column contains the time of arrival (TOA) of the candidates, computed with respect to the topocentric reference frame and at a frequency v_top = 1582 MHz. Columns three and four contain the Right Ascension (R.A.) and Declination (Dec.) beam pointings where the burst occurred. The fifth column represents the DM of the bursts, while the sixth column contains the DM prediction of the Galactic contribution based on the NE2001 (Cordes & Lazio 2002) or YMW16 (Yao et al. 2017) models, whichever is the highest for that pointing. Δt is the FWHM time width of the bursts, computed via a Gaussian fit, corrected for intra-channel smearing and sampling time. As the scattering contribution is not resolved for most bursts, these widths are reported as upper limits. The eighth column reports the discovery sub-band. v₀ and Δv in the ninth and tenth columns are the frequency centroid and FWHM width, respectively, obtained via a Gaussian fit. For the FRBs that cover the full observational band, the frequency centroid has been assigned to the central frequency of the PMB, and the observational bandwidth is reported as the lower limit to the effective bandwidth of the burst. Bursts for which the Gaussian frequency fit did not converge have the detection sub-band central frequency and width reported instead. S/N* represents the signal-to-noise ratio computed with respect to the discovery band for each burst. F_v is the fluence computed via the radiometer equation. Note that these values should be considered as lower limits, as we assumed the telescope gain at the central beam of the PMB in the radiometer equation. References: [1] Thornton et al. (2013), [2] Champion et al. (2016), [3] Petroff et al. (2019), [4] This work.