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The LIGO-Virgo-KAGRA (LVK) Collaboration has reported nearly 100 BH-BHmergers. The LVK provides estimates of rates, masses, effective spins, andredshifts for these mergers. Yet, the formation channel(s) of the mergersremains uncertain. One way to search for a formation site is to contrastproperties of detected BH-BH mergers with different models of BH-BH mergerformation. Our study is designed to investigate the usefulness of the totalBH-BH merger mass and its evolution with redshift in establishing the origin ofgravitational-wave sources. We find that the average intrinsic BH-BH totalmerger mass shows exceptionally different behavior for the models that we adoptfor our analysis. In the local universe (z=0) the average merger mass changesfrom Mtot,int=25Msun for CE binary evolution and open clusters formationchannels, to Mtot,int=30Msun for the stable-RLOF binary channel, toMtot,int=45Msun for the globular cluster channel. These differences are evenmore pronounced at larger redshifts. However, these differences are diminishedwhen considering LVK O3 detector sensitivity. Comparison with LVK O3 data showsthat none of our adopted models can match the data despite large errors onBH-BH masses and redshifts. We emphasize that our conclusions are derived froma small set of 6 models that are subject to numerous known uncertainties. Wealso note that BH-BH mergers may originate from a mix of several channels andthat other (than those adopted here) BH-BH formation channels may exist.

Black hole - black hole total merger mass and the origin of LIGO/Virgo sources