Forward Modelling the O3(a+b) GW transient mass distributions with BPASS by varying compact remnant mass and SNe kick prescriptions. (arXiv:2105.05783v4 [astro-ph.HE] UPDATED)
<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 modeling from the BPASS code suite of the population of
observed gravitational wave (GW) transients reported by the LIGO/VIRGO
consortium (LVC) during their third observing run, O3(a+b). 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 O3(a+b). We investigate how
these predictions change by alternating between four different remnant mass
estimation schemes and two supernovae (SNe) kick prescriptions. We find that
none of the model populations resulting from these variations accurately match
the whole O3(a+b) 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 (BHs) close to the mass gap, while
also increasing the number of higher mass BHs below the pair-instability SN
limit. Finally, we find that the interaction between the value of the remnant
mass from a stellar model and the choice of SN kick is complex and different
kick prescriptions may be required depending on whether a neutron star or BH is
formed.
We present forward modeling from the BPASS code suite of the population of
observed gravitational wave (GW) transients reported by the LIGO/VIRGO
consortium (LVC) during their third observing run, O3(a+b). 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 O3(a+b). We investigate how
these predictions change by alternating between four different remnant mass
estimation schemes and two supernovae (SNe) kick prescriptions. We find that
none of the model populations resulting from these variations accurately match
the whole O3(a+b) 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 (BHs) close to the mass gap, while
also increasing the number of higher mass BHs below the pair-instability SN
limit. Finally, we find that the interaction between the value of the remnant
mass from a stellar model and the choice of SN kick is complex and different
kick prescriptions may be required depending on whether a neutron star or BH is
formed.
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