  The primary and secondary masses of the binary black holes (BBH) reported by
LIGO/Virgo are correlated with a narrow dispersion that appears to increase in
proportion to mass. The mean binary mass ratio $1.45\pm0.07$ we show is
consistent with pairs drawn randomly from the mass distribution of black holes
in our Galaxy. However, BBH masses are concentrated around $\simeq 30M_\odot$,
whereas black holes in our Galaxy peak at $\simeq 10M_\odot$. This mass
difference can be reconciled by gravitational lensing magnification which
allows distant events to be detected with typically $z\simeq 2$, so the
waveform is reduced in frequency by $1+z$, and hence the measured chirp masses
appear 3 times larger than their intrinsic values. This redshift enhancement
also accounts for the dispersion of primary and secondary masses, both of which
should increase as $1+z$, thereby appearing to scale with mass, in agreement
with the data. Thus the BBH component masses provide independent support for
lensing, implying most high chirp mass events have intrinsic masses like the
stellar mass black holes in our Galaxy, coalescing at $z>1$, with only two low
mass BBH detections, of $\simeq 10M_\odot$ as expected for unlensed events in
the local Universe, $z\simeq 0.1$. This lensing solution requires a rapidly
declining BBH event rate below $z<1$, which together with the observed absence
of BBH spin suggests most events originate within young globular clusters at
$z>1$, via efficient binary capture of stellar mass black holes with randomly
oriented spins.
