Observation of eccentric binary black hole mergers with second and third generation gravitational wave detector networks. (arXiv:2008.03313v1 [gr-qc])

Observation of eccentric binary black hole mergers with second and third generation gravitational wave detector networks. (arXiv:2008.03313v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Chen_Z/0/1/0/all/0/1">Zhuo Chen</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Huerta_E/0/1/0/all/0/1">E. A. Huerta</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Adamo_J/0/1/0/all/0/1">Joseph Adamo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Haas_R/0/1/0/all/0/1">Roland Haas</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+OShea_E/0/1/0/all/0/1">Eamonn O&#x27;Shea</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Kumar_P/0/1/0/all/0/1">Prayush Kumar</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Moore_C/0/1/0/all/0/1">Chris Moore</a>

[Abridged] We introduce an improved version of the Eccentric, Non-spinning,
Inspiral-Gaussian-process Merger Approximant (ENIGMA) waveform model. We find
that this ready-to-use model can: (i) produce physically consistent signals
when sampling over 1M samples chosen over the
$m_{{1,,2}}in[5M_{odot},,50M_{odot}]$ parameter space, and the entire
range of binary inclination angles; (ii) produce waveforms within 0.04 seconds
from an initial gravitational wave frequency $f_{textrm{GW}} =15,textrm{Hz}$
and at a sample rate of 8192 Hz; and (iii) reproduce the physics of
quasi-circular mergers. We utilize ENIGMA to compute the expected
signal-to-noise ratio (SNR) distributions of eccentric binary black hole
mergers assuming the existence of second and third generation gravitational
wave detector networks that include the twin LIGO detectors, Virgo, KAGRA,
LIGO-India, a LIGO-type detector in Australia, Cosmic Explorer, and the
Einstein Telescope. In the context of advanced LIGO-type detectors, we find
that the SNR of eccentric mergers is always larger than quasi-circular mergers
for systems with $e_0leq0.4$ at $f_{textrm{GW}} =10,textrm{Hz}$, even if
the timespan of eccentric signals is just a third of quasi-circular systems
with identical total mass and mass-ratio. For Cosmic Explorer-type detector
networks, we find that eccentric mergers have similar SNRs than quasi-circular
systems for $e_0leq0.3$ at $f_{textrm{GW}} =10,textrm{Hz}$. Systems with
$e_0sim0.5$ at $f_{textrm{GW}} =10,textrm{Hz}$ have SNRs that range between
50%-90% of the SNR produced by quasi-circular mergers, even if these eccentric
signals are just between a third to a tenth the length of quasi-circular
systems. For Einstein Telescope-type detectors, we find that eccentric mergers
have similar SNRs than quasi-circular systems for $e_0leq0.4$ at
$f_{textrm{GW}} =5,textrm{Hz}$.

[Abridged] We introduce an improved version of the Eccentric, Non-spinning,
Inspiral-Gaussian-process Merger Approximant (ENIGMA) waveform model. We find
that this ready-to-use model can: (i) produce physically consistent signals
when sampling over 1M samples chosen over the
$m_{{1,,2}}in[5M_{odot},,50M_{odot}]$ parameter space, and the entire
range of binary inclination angles; (ii) produce waveforms within 0.04 seconds
from an initial gravitational wave frequency $f_{textrm{GW}} =15,textrm{Hz}$
and at a sample rate of 8192 Hz; and (iii) reproduce the physics of
quasi-circular mergers. We utilize ENIGMA to compute the expected
signal-to-noise ratio (SNR) distributions of eccentric binary black hole
mergers assuming the existence of second and third generation gravitational
wave detector networks that include the twin LIGO detectors, Virgo, KAGRA,
LIGO-India, a LIGO-type detector in Australia, Cosmic Explorer, and the
Einstein Telescope. In the context of advanced LIGO-type detectors, we find
that the SNR of eccentric mergers is always larger than quasi-circular mergers
for systems with $e_0leq0.4$ at $f_{textrm{GW}} =10,textrm{Hz}$, even if
the timespan of eccentric signals is just a third of quasi-circular systems
with identical total mass and mass-ratio. For Cosmic Explorer-type detector
networks, we find that eccentric mergers have similar SNRs than quasi-circular
systems for $e_0leq0.3$ at $f_{textrm{GW}} =10,textrm{Hz}$. Systems with
$e_0sim0.5$ at $f_{textrm{GW}} =10,textrm{Hz}$ have SNRs that range between
50%-90% of the SNR produced by quasi-circular mergers, even if these eccentric
signals are just between a third to a tenth the length of quasi-circular
systems. For Einstein Telescope-type detectors, we find that eccentric mergers
have similar SNRs than quasi-circular systems for $e_0leq0.4$ at
$f_{textrm{GW}} =5,textrm{Hz}$.

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