Dynamical formation of the GW190814 merger. (arXiv:2102.03364v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Sedda_M/0/1/0/all/0/1">Manuel Arca Sedda</a>
We investigate the possible dynamical origin of GW190814, a gravitational
wave (GW) source discovered by the LIGO-Virgo-Kagra collaboration (LVC)
associated with a merger between a stellar black hole (BH) with mass $23.2$
M$_odot$ and a compact object, either a BH or a neutron star (NS), with mass
$2.59$ M$_odot$. Using a database of 240,000 $N$-body simulations modelling
the formation of NS-BH mergers via dynamical encounters in dense clusters, we
find that systems like GW190814 are likely to form in young, metal-rich
clusters. Our model suggests that a little excess ($sim 2-4%$) of objects
with masses in the range $2.3-3$ M$_odot$ in the compact remnants mass
spectrum leads to a detection rate for dynamically formed “GW190814 -like”
mergers of $Gamma_{rm GW190814} simeq 1-6$ yr Gpc$^{-3}$, i.e. within the
observational constraints set by the GW190814 discovery, $Gamma_{rm LVC} sim
1-23$ yr Gpc$^{-3}$. Additionally, our model suggests that $sim 1.8-4.8%$ of
dynamical NS-BH mergers are compatible with GW190426_152155, the only
confirmed NS-BH merger detected by the LVC. We show that the relative amount of
light and heavy NS-BH mergers can provide clues about the environments in which
they developed.
We investigate the possible dynamical origin of GW190814, a gravitational
wave (GW) source discovered by the LIGO-Virgo-Kagra collaboration (LVC)
associated with a merger between a stellar black hole (BH) with mass $23.2$
M$_odot$ and a compact object, either a BH or a neutron star (NS), with mass
$2.59$ M$_odot$. Using a database of 240,000 $N$-body simulations modelling
the formation of NS-BH mergers via dynamical encounters in dense clusters, we
find that systems like GW190814 are likely to form in young, metal-rich
clusters. Our model suggests that a little excess ($sim 2-4%$) of objects
with masses in the range $2.3-3$ M$_odot$ in the compact remnants mass
spectrum leads to a detection rate for dynamically formed “GW190814 -like”
mergers of $Gamma_{rm GW190814} simeq 1-6$ yr Gpc$^{-3}$, i.e. within the
observational constraints set by the GW190814 discovery, $Gamma_{rm LVC} sim
1-23$ yr Gpc$^{-3}$. Additionally, our model suggests that $sim 1.8-4.8%$ of
dynamical NS-BH mergers are compatible with GW190426_152155, the only
confirmed NS-BH merger detected by the LVC. We show that the relative amount of
light and heavy NS-BH mergers can provide clues about the environments in which
they developed.
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