List of Footnotes

1 Pulsar astronomers usually define the luminosity L = Sd2, where S is the mean flux density at 400 MHz (a standard observing frequency) and d is the distance derived from the DM (see Section 2.4). Since this ignores any assumptions about beaming or geometrical factors, it is sometimes referred to as a “pseudoluminosity” [8].
2 The likely DNS binary J1756-2251 [93Jump To The Next Citation Point] has a merger time of 1.7 Gyr and will make a small contribution to the rate. It has so far not been incorporated into the latest calculations.
3 It is likely, however, that a more detailed statistical analysis of the data are required to confirm or refute this result [82].