Gravitational-wave detection rates for compact binaries formed in isolation: LIGO/Virgo O3 and beyond. (arXiv:1906.04197v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Baibhav_V/0/1/0/all/0/1">Vishal Baibhav</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Berti_E/0/1/0/all/0/1">Emanuele Berti</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Gerosa_D/0/1/0/all/0/1">Davide Gerosa</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Mapelli_M/0/1/0/all/0/1">Michela Mapelli</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Giacobbo_N/0/1/0/all/0/1">Nicola Giacobbo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bouffanais_Y/0/1/0/all/0/1">Yann Bouffanais</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Carlo_U/0/1/0/all/0/1">Ugo N. Di Carlo</a>
Using simulations performed with the population synthesis code MOBSE, we
compute the merger rate densities and detection rates of compact binary mergers
formed in isolation for second- and third-generation gravitational-wave
detectors. We estimate how rates are affected by uncertainties on key
stellar-physics parameters, namely common envelope evolution and natal kicks.
We estimate how future upgrades will increase the size of the available catalog
of merger events, and we discuss features of the merger rate density that will
become accessible with third-generation detectors.
Using simulations performed with the population synthesis code MOBSE, we
compute the merger rate densities and detection rates of compact binary mergers
formed in isolation for second- and third-generation gravitational-wave
detectors. We estimate how rates are affected by uncertainties on key
stellar-physics parameters, namely common envelope evolution and natal kicks.
We estimate how future upgrades will increase the size of the available catalog
of merger events, and we discuss features of the merger rate density that will
become accessible with third-generation detectors.
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