The paper updates constraints on primordial black hole (PBH) abundance using data from the third observational run (O3) of the LIGO-Virgo-KAGRA (LVK) experiment. The authors apply a hierarchical Bayesian analysis to a population of binaries consisting of both primordial and astrophysical black holes. They consider various mass functions, including critical collapse in the QCD epoch and primordial non-Gaussianities. The results show that in all scenarios, the PBH abundance is constrained to be at most \( f_{\text{PBH}} \lesssim 10^{-3} \) for masses in the range \( 1 - 200 M_{\odot} \). The shape and strength of the constraints are not significantly affected by the type of non-Gaussianities, modifications to the mass function during the QCD epoch, or the modeling of the astrophysical PBH population. The paper also discusses the impact of different mass functions and the contribution from PBH binaries formed from three-body systems in the early universe. Overall, the constraints are insensitive to the detailed shape of the mass function and the modeling of astrophysical black holes.The paper updates constraints on primordial black hole (PBH) abundance using data from the third observational run (O3) of the LIGO-Virgo-KAGRA (LVK) experiment. The authors apply a hierarchical Bayesian analysis to a population of binaries consisting of both primordial and astrophysical black holes. They consider various mass functions, including critical collapse in the QCD epoch and primordial non-Gaussianities. The results show that in all scenarios, the PBH abundance is constrained to be at most \( f_{\text{PBH}} \lesssim 10^{-3} \) for masses in the range \( 1 - 200 M_{\odot} \). The shape and strength of the constraints are not significantly affected by the type of non-Gaussianities, modifications to the mass function during the QCD epoch, or the modeling of the astrophysical PBH population. The paper also discusses the impact of different mass functions and the contribution from PBH binaries formed from three-body systems in the early universe. Overall, the constraints are insensitive to the detailed shape of the mass function and the modeling of astrophysical black holes.