Extended Data Table 3 Burst properties

From: A link between repeating and non-repeating fast radio bursts through their energy distributions

  1. See text for details on how the values were derived. Footnotes:
  2. aTime of arrival at the solar system barycenter at infinite frequency in TDB (using a DM of 410.8 pc cm−3, a dispersion measure constant of 1/0.000241 GHz2 cm3 pc−1 μs and as (J2000) position RA = 05:08:03.5, Dec = +26:03:37.8; for times marked with a *, a DM constant of 4.14880568679703 GHz2cm3pc−1ms was used). For multi-component busts, the TOA is defined as the middle between the peak of the first and the last component.
  3. bThe peak S/N of the brightest component.
  4. cComputed as the sum over the measured fluence of each component. We assume a conservative error of 20% for all bursts, dominated by the uncertainty of the SEFD.
  5. dManually determined time span between start of first and end of last component.
  6. eComputed using DL=453 Mpc, z=0.098 and the listed width.
  7. fBandwidth used for computing the fluence. This is often the full available observing bandwidth.
  8. gWeighted average over the measured scintillation bandwidth per component.
  9. hNo measurement was possible due to low S/N.
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