Forward Modelling the LIGO/VIRGO O3a GW transient mass distributions with BPASS. (arXiv:2105.05783v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ghodla_S/0/1/0/all/0/1">Sohan Ghodla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zeist_W/0/1/0/all/0/1">Wouter G.J. van Zeist</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eldridge_J/0/1/0/all/0/1">J.J. Eldridge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevance_H/0/1/0/all/0/1">Héloïse F. Stevance</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanway_E/0/1/0/all/0/1">Elizabeth R. Stanway</a>
We present forward modelling from the BPASS code suite of the population of
observed gravitational wave (GW) transients from the first half of the third
LIGO/VIRGO consortium (LVC) observing run (O3a). Specifically, we predict the
expected chirp mass and mass ratio distributions for GW transients, taking
account of detector sensitivity to determine how many events should have been
detected by the current detector network in O3a. We investigate how the
predictions change by comparing four different schemes for estimating the final
remnant masses from our stellar evolution models and two different supernova
kick prescriptions. We find that none of our model populations accurately match
the whole O3a GW transient catalog. However, agreement from some models to part
of the catalog suggests ways to achieve a more complete fit. These include
reducing the number of low mass black holes close to the mass gap, while also
increasing the number of higher mass black holes below the pair-instability
supernova limit. Finally, we find that the interaction between the value of
remnant mass from a stellar model and the choice of supernova kick is complex
and different kick models may be required depending on whether a neutron star
or black hole is formed.
We present forward modelling from the BPASS code suite of the population of
observed gravitational wave (GW) transients from the first half of the third
LIGO/VIRGO consortium (LVC) observing run (O3a). Specifically, we predict the
expected chirp mass and mass ratio distributions for GW transients, taking
account of detector sensitivity to determine how many events should have been
detected by the current detector network in O3a. We investigate how the
predictions change by comparing four different schemes for estimating the final
remnant masses from our stellar evolution models and two different supernova
kick prescriptions. We find that none of our model populations accurately match
the whole O3a GW transient catalog. However, agreement from some models to part
of the catalog suggests ways to achieve a more complete fit. These include
reducing the number of low mass black holes close to the mass gap, while also
increasing the number of higher mass black holes below the pair-instability
supernova limit. Finally, we find that the interaction between the value of
remnant mass from a stellar model and the choice of supernova kick is complex
and different kick models may be required depending on whether a neutron star
or black hole is formed.
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