![]() ![]() ![]() ![]() The favorable comparison of the existing LIGO/Virgo observations with our model predictions gives support to the idea that the majority, if not all of the observed mergers, originate from the evolution of isolated binaries. Moreover, we find that M chirp and χ eff distributions are very weakly dependent on the detector sensitivity.Ĭonclusions. We expect approximately 80% of events with χ eff < 0.1, while the remaining 20% of events with χ eff ≥ 0.1 are split into ∼10% with M chirp < 15 M ⊙ and ∼10% with M chirp ≥ 15 M ⊙. We make predictions for the third observing run O3 and for Advanced LIGO design sensitivity. We find an excellent agreement between our model and the ten events from the first two advanced detector observing runs. By assuming efficient angular momentum transport, we are able to present a model that is capable of simultaneously predicting the following three main gravitational-wave observables: the effective inspiral spin parameter χ eff, the chirp mass M chirp and the cosmological redshift of merger z merger. We then convolved our binary evolution calculations with the redshift- and metallicity-dependent star-formation rate and the selection effects of gravitational-wave detectors to obtain predictions of observable properties. To achieve this aim, we used a hybrid technique that combines the parametric binary population synthesis code COMPAS with detailed binary evolution simulations performed with the MESA code. We study the formation of coalescing binary black holes via the evolution of isolated field binaries that go through the common envelope phase in order to obtain the combined distributions of observables such as black-hole spins, masses and cosmological redshifts of mergers. As more merger detections are expected with future gravitational-wave observations, population synthesis studies can help to distinguish between them.Īims. Several formation channels for merging black holes have been proposed in the literature. After years of scientific progress, the origin of stellar binary black holes is still a great mystery. Niels Bohr Institute, University of Copenhagen, BlegdamsCopenhagen, DenmarkĬenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USAĬentre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, AustraliaĬontext. Crédito Constructor, Ciudad de México 03940, Mexico Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, MexicoĬonsejo Nacional de Ciencia y Tecnología, Av. Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Clayton, Victoria 3800, AustraliaĪRC Centre of Excellence for Gravitational Wave Discovery – OzGrav, Australia Geneva Observatory, University of Geneva, Chemin des MailletVersoix, SwitzerlandĮ-mail: Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK Gaebel 2, Chase Kimball 8 and Simon Stevenson 9 ,4 ![]() Neijssel 2, Ilya Mandel 3 ,2 ,4, Aldo Batta 5 ,6 ,7, Sebastian M. Bavera 1, Tassos Fragos 1, Ying Qin 1, Emmanouil Zapartas 1, Coenraad J. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes ![]()
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