Calibrating the binary black hole population in nuclear star clusters through tidal disruption events. (arXiv:2006.14632v1 [astro-ph.GA])

Calibrating the binary black hole population in nuclear star clusters through tidal disruption events. (arXiv:2006.14632v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Fragione_G/0/1/0/all/0/1">Giacomo Fragione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perna_R/0/1/0/all/0/1">Rosalba Perna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a>

As the sensitivity of gravitational wave (GW) instruments improves and new
networks start operating, hundreds of merging stellar-mass black holes (SBHs)
and intermediate-mass black holes (IMBHs) are expected to be observed in the
next few years. The origin and distribution of SBH and IMBH binaries in various
dynamical environments is a fundamental scientific question in GW astronomy. In
this paper we discuss the electromagnetic window provided by tidal disruption
events (TDEs) of stars, into the assembly and merger of binary SBHs and IMBHs
in nuclear star clusters (NSCs). We discuss how the host NSC mass and density
and the slope of the black-hole mass function set the orbital properties and
the masses of the binaries that undergo a TDE. For typical NSC properties, we
predict a merger rate of $sim 10^{-6}$–$10^{-7} {rm yr}^{-1}$ per galaxy.
The lightcurve of TDEs in NSCs could be interrupted and modulated by the
companion black hole on the orbital period of the binary. The ejected mass
associated with TDEs can produce optical transients of luminosity $sim
10^{42}$–$10^{44}$ erg s$^{-1}$ over timescales of days to months. These
should be readily detectable by optical transient surveys such as the Zwicky
Transient Facility and LSST.

As the sensitivity of gravitational wave (GW) instruments improves and new
networks start operating, hundreds of merging stellar-mass black holes (SBHs)
and intermediate-mass black holes (IMBHs) are expected to be observed in the
next few years. The origin and distribution of SBH and IMBH binaries in various
dynamical environments is a fundamental scientific question in GW astronomy. In
this paper we discuss the electromagnetic window provided by tidal disruption
events (TDEs) of stars, into the assembly and merger of binary SBHs and IMBHs
in nuclear star clusters (NSCs). We discuss how the host NSC mass and density
and the slope of the black-hole mass function set the orbital properties and
the masses of the binaries that undergo a TDE. For typical NSC properties, we
predict a merger rate of $sim 10^{-6}$–$10^{-7} {rm yr}^{-1}$ per galaxy.
The lightcurve of TDEs in NSCs could be interrupted and modulated by the
companion black hole on the orbital period of the binary. The ejected mass
associated with TDEs can produce optical transients of luminosity $sim
10^{42}$–$10^{44}$ erg s$^{-1}$ over timescales of days to months. These
should be readily detectable by optical transient surveys such as the Zwicky
Transient Facility and LSST.

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