On mass distribution of coalescing black holes. (arXiv:2005.00892v1 [astro-ph.CO])

On mass distribution of coalescing black holes. (arXiv:2005.00892v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dolgov_A/0/1/0/all/0/1">A. D. Dolgov</a> (Novosibirsk U., ITEP Moscow), <a href="http://arxiv.org/find/astro-ph/1/au:+Kuranov_A/0/1/0/all/0/1">A.G. Kuranov</a> (Sternberg Astron. Inst.), <a href="http://arxiv.org/find/astro-ph/1/au:+Mitichkin_N/0/1/0/all/0/1">N.A. Mitichkin</a> (Faculty of Physics, Moscow U.), <a href="http://arxiv.org/find/astro-ph/1/au:+Porey_S/0/1/0/all/0/1">S. Porey</a> (Novosibirsk U.), <a href="http://arxiv.org/find/astro-ph/1/au:+Postnov_K/0/1/0/all/0/1">K.A. Postnov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sazhina_O/0/1/0/all/0/1">O.S. Sazhina</a> (Sternberg Astron. Inst.), <a href="http://arxiv.org/find/astro-ph/1/au:+Simkin_I/0/1/0/all/0/1">I.V. Simkin</a> (Bauman Technical U., Moscow)

The available data on the chirp mass distribution of the black holes in the
coalescing binaries in O1-O3 LIGO/Virgo runs are analyzed and compared with
theoretical expectations based on the hypothesis that these black holes are
primordial with log-normal mass spectrum. The inferred best-fit mass spectrum
parameters, $M_0=17 M_odot$ and $gamma=0.9$, fall within the theoretically
expected range and shows excellent agreement with observations. On the
opposite, binary black hole models based on massive binary star evolution
require additional adjustments to reproduce the observed chirp mass
distribution.

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