Prospects for Future Binary Black Hole GW Studies in Light of PTA Measurements. (arXiv:2301.13854v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ellis_J/0/1/0/all/0/1">John Ellis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fairbairn_M/0/1/0/all/0/1">Malcolm Fairbairn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hutsi_G/0/1/0/all/0/1">Gert Hütsi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raidal_M/0/1/0/all/0/1">Martti Raidal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urrutia_J/0/1/0/all/0/1">Juan Urrutia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaskonen_V/0/1/0/all/0/1">Ville Vaskonen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veermae_H/0/1/0/all/0/1">Hardi Veermäe</a>
NANOGrav and other Pulsar Timing Arrays (PTAs) have discovered a
common-spectrum process in the nHz range that may be due to gravitational waves
(GWs): if so, they are likely to have been generated by black hole (BH)
binaries with total masses $> 10^9 M_{odot}$. Using the Extended
Press-Schechter formalism to model the galactic halo mass function and a simple
relation between the halo and BH masses suggests that these binaries have
redshifts $z = {cal O}(1)$ and mass ratios $gtrsim 10$, and that the GW
signal at frequencies above ${cal O}(10)$~nHz may be dominated by relatively
few binaries that could be distinguished experimentally and would yield
observable circular polarization. Extrapolating the model to higher frequencies
indicates that future GW detectors such as LISA and AEDGE could extend the PTA
observations to lower BH masses $in (10^6, 10^9 ) M_{odot}$ and $in (10^3,
10^9) M_{odot}$.
NANOGrav and other Pulsar Timing Arrays (PTAs) have discovered a
common-spectrum process in the nHz range that may be due to gravitational waves
(GWs): if so, they are likely to have been generated by black hole (BH)
binaries with total masses $> 10^9 M_{odot}$. Using the Extended
Press-Schechter formalism to model the galactic halo mass function and a simple
relation between the halo and BH masses suggests that these binaries have
redshifts $z = {cal O}(1)$ and mass ratios $gtrsim 10$, and that the GW
signal at frequencies above ${cal O}(10)$~nHz may be dominated by relatively
few binaries that could be distinguished experimentally and would yield
observable circular polarization. Extrapolating the model to higher frequencies
indicates that future GW detectors such as LISA and AEDGE could extend the PTA
observations to lower BH masses $in (10^6, 10^9 ) M_{odot}$ and $in (10^3,
10^9) M_{odot}$.
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