  The first and second Gravitational Wave Transient Catalogs by the LIGO/Virgo
Collaboration include $50$ confirmed merger events from the first, second, and
first half of the third observational runs. We compute the distribution of
recoil kicks imparted to the merger remnants and estimate their retention
probability within various astrophysical environments as a function of the
maximum progenitor spin ($\chi_{\rm max}$), assuming that the LIGO/Virgo binary
black hole (BBH) mergers were catalyzed by dynamical assembly in a dense star
cluster. We find that the distributions of average recoil kicks are peaked at
about $150$ km s$^{-1}$, $250$ km s$^{-1}$, $350$ km s$^{-1}$, $600$ km
s$^{-1}$, for maximum progenitor spins of $0.1$, $0.3$, $0.5$, $0.8$,
respectively. Only environments with escape speed $\gtrsim 100$ km s$^{-1}$, as
found in galactic nuclear star clusters as well as in the most massive globular
clusters and super star clusters, could efficiently retain the merger remnants
of the LIGO/Virgo BBH population even for low progenitor spins ($\chi_{\rm
max}=0.1$). In the case of high progenitor spins ($\chi_{\rm max}\gtrsim 0.5$),
only the most massive nuclear star clusters can retain the merger products. We
also show that the estimated values of the effective spin and of the remnant
spin of GW170729, GW190412, GW190519, and GW190620 can be reproduced if their
progenitors were moderately spinning ($\chi_{\rm max}\gtrsim 0.3$), while for
GW190517 if the progenitors were rapidly spinning ($\chi_{\rm max}\gtrsim
0.8$). Alternatively, some of these events could be explained if at least one
of the progenitors is already a second-generation BH, originated from a
previous merger.
