Effect of eccentricity on binary neutron star searches in advanced LIGO

Huerta, E. A.; Brown, D. A.

doi:10.1103/physrevd.87.127501

Cited by 84 publications

(101 citation statements)

References 47 publications

(68 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These studies have shown that detecting and characterizing eccentric binary systems will not be feasible using existing algorithms for quasicircular binaries [33,72]. Furthermore, as discussed in Ref.…”

Section: Introductionmentioning

confidence: 98%

Complete waveform model for compact binaries on eccentric orbits

et al. 2017

View full text Add to dashboard Cite

We present a time domain waveform model that describes the inspiral, merger and ringdown of compact binary systems whose components are nonspinning, and which evolve on orbits with low to moderate eccentricity. The inspiral evolution is described using third-order post-Newtonian equations both for the equations of motion of the binary, and its far-zone radiation field. This latter component also includes instantaneous, tails and tails-of-tails contributions, and a contribution due to nonlinear memory. This framework reduces to the post-Newtonian approximant TaylorT4 at third postNewtonian order in the zero-eccentricity limit. To improve phase accuracy, we also incorporate higher-order post-Newtonian corrections for the energy flux of quasicircular binaries and gravitational self-force corrections to the binding energy of compact binaries. This enhanced prescription for the inspiral evolution is combined with a fully analytical prescription for the merger-ringdown evolution constructed using a catalog of numerical relativity simulations. We show that this inspiral-mergerringdown waveform model reproduces the effective-one-body model of Ref. [Y. Pan et al., Phys. Rev. D 89, 061501 (2014).] for quasicircular black hole binaries with mass ratios between 1 to 15 in the zero-eccentricity limit over a wide range of the parameter space under consideration. Using a set of eccentric numerical relativity simulations, not used during calibration, we show that our new eccentric model reproduces the true features of eccentric compact binary coalescence throughout merger. We use this model to show that the gravitational-wave transients GW150914 and GW151226 can be effectively recovered with template banks of quasicircular, spin-aligned waveforms if the eccentricity e 0 of these systems when they enter the aLIGO band at a gravitational-wave frequency of 14 Hz satisfies e GW150914 0 ≤ 0.15 and e GW151226 0 ≤ 0.1. We also find that varying the spin combinations of the quasicircular, spin-aligned template waveforms does not improve the recovery of nonspinning, eccentric signals when e 0 ≥ 0.1. This suggests that these two signal manifolds are predominantly orthogonal.

show abstract

Section: Introductionmentioning

confidence: 98%

Complete waveform model for compact binaries on eccentric orbits

et al. 2017

View full text Add to dashboard Cite

show abstract

“…Huerta and Brown estimate signal-to-noise ratio loss factors of about 0.5 and 0.2 for BNS systems with eccentricities of 0.2 and 0.4 respectively [11]. This would bring the matched filtering sensitivity distances of these signals to 225 Mpc and 90 Mpc, compared to 160 Mpc for these two eccentricity values when using seedless clustering; therefore seedless clustering with eccentric template banks may provide further opportunities for observing these types of signals.…”

Section: Discussionmentioning

confidence: 99%

“…Up until now, there have been no dedicated matched filtering searches for low a Electronic address: coughlin@physics.harvard.edu b Electronic address: meyers@physics.umn.edu mass binaries with low to moderate eccentricities. Huerta and Brown have shown that searches using waveforms that assume no eccentricity are significantly sub-optimal above > 0.05 [11]. They conclude that in order to detect and study the rate of eccentric stellar-mass compact binaries in aLIGO, a search specifically targeting these systems will need to be constructed.…”

Section: Introductionmentioning

confidence: 99%

Detectability of eccentric compact binary coalescences with advanced gravitational-wave detectors

et al. 2015

View full text Add to dashboard Cite

Compact binary coalescences are a promising source of gravitational waves for second-generation interferometric gravitational-wave detectors such as advanced LIGO and advanced Virgo. While most binaries are expected to possess circular orbits, some may be eccentric, for example, if they are formed through dynamical capture. Eccentric orbits can create difficulty for matched filtering searches due to the challenges of creating effective template banks to detect these signals. In previous work, we showed how seedless clustering can be used to detect low-mass (M total ≤ 10M ) compact binary coalescences for both spinning and eccentric systems, assuming a circular postNewtonian expansion. Here, we describe a parameterization that is designed to maximize sensitivity to low-eccentricity (0 ≤ ≤ 0.6) systems, derived from the analytic equations. We show that this parameterization provides a robust and computationally efficient method for detecting eccentric low-mass compact binaries. Based on these results, we conclude that advanced detectors will have a chance of detecting eccentric binaries if optimistic models prove true. However, a null observation is unlikely to firmly rule out models of eccentric binary populations.

show abstract

“…Ultimately gravitational wave observations will be the primary tool to measure eccentricity of compact object inspirals and to constrain the rate of eccentric compact mergers. Unfortunately, the present detection template bank used by LIGO is entirely circular [5,52], hindering detection of systems with in-band eccentricities above about e ∼ 0.1 [25,53,54]. Due to this same absence of eccentric waveform models, parameter estimation must likewise assume quasi-circularity.…”

Section: Introductionmentioning

confidence: 99%

Fundamental frequencies and resonances from eccentric and precessing binary black hole inspirals

Lewis

Zimmerman

Pfeiffer

2017

Class. Quantum Grav.

View full text Add to dashboard Cite

Abstract. Binary black holes which are both eccentric and undergo precession remain unexplored in numerical simulations. We present simulations of such systems which cover about 50 orbits at comparatively high mass ratios 5 and 7. The configurations correspond to the generic motion of a nonspinning body in a Kerr spacetime, and are chosen to study the transition from finite mass-ratio inspirals to point particle motion in Kerr. We develop techniques to extract analogs of the three fundamental frequencies of Kerr geodesics, compare our frequencies to those of Kerr, and show that the differences are consistent with self-force corrections entering at first order in mass ratio. This analysis also locates orbital resonances where the ratios of our frequencies take rational values. At the considered mass ratios, the binaries pass through resonances in one to two resonant cycles, and we find no discernible effects on the orbital evolution. We also compute the decay of eccentricity during the inspiral and find good agreement with the leading order post-Newtonian prediction.

show abstract

Effect of eccentricity on binary neutron star searches in advanced LIGO

Cited by 84 publications

References 47 publications

Complete waveform model for compact binaries on eccentric orbits

Complete waveform model for compact binaries on eccentric orbits

Detectability of eccentric compact binary coalescences with advanced gravitational-wave detectors

Fundamental frequencies and resonances from eccentric and precessing binary black hole inspirals

Contact Info

Product

Resources

About