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'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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