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A geometric template bank for the detection of spinning low-mass compact binaries with moderate orbital eccentricity

T0 review · 2 major / 6 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Modelled searches with quasi-circular template banks miss more than 40% of moderately eccentric binary neutron star and neutron star–black hole signals; a new geometric bank that adds eccentricity as a template dimension recovers over 94%…

desk verdict First geometric template bank for eccentric aligned-spin BNS/NSBH, with solid within-model validation and a clear control experiment; the headline miss rates are model-internal and the paper says so, if not loudly enough. read the letter →

arxiv 2412.06433 v3 pith:EHRZFWK2 submitted 2024-12-09 gr-qc astro-ph.HEastro-ph.IM

Khun Sang Phukon , Patricia Schmidt , Geraint Pratten This is my paper · ORCID
classification gr-qcastro-ph.HEastro-ph.IM MSC 83C35 PACS 04.30.-w
keywords geometrictemplatebankgravitationalwavesorbitaleccentricitymatchedfilteringbinaryneutronstarstar–blackholeTaylorF2Eccpost-Newtonianmetric
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper argues that modelled gravitational-wave searches using quasi-circular template banks are badly mismatched to real binary neutron star (BNS) and neutron star–black hole (NSBH) signals with even moderate orbital eccentricity. For eccentricities $e_0$ in $[10^{-5},0.15]$ defined at 15 Hz, such banks lose more than 25% of detectable signals at $e_0\approx 0.1$ and more than 40% at the highest values, producing a strong selection bias against dynamically formed binaries. The authors construct the first geometric template bank that adds eccentricity as an explicit search dimension for aligned-spin low-mass binaries, based on the post-Newtonian inspiral model TaylorF2Ecc. The resulting 4.78-million-template bank misses fewer than 6% of eccentric injections because of finite template spacing, and the improvement is shown to come from the eccentricity dimension rather than from the larger bank size. If correct, this makes a modelled search for moderately eccentric BNS/NSBH mergers computationally practical.

What carries the argument

The machinery is a globally flat matched-filter metric constructed in the space of TaylorF2Ecc phase coefficients. The waveform phase is split into quasi-circular and eccentric pieces, each expanded in powers of $x=f/70\,\mathrm{Hz}$, giving 13 dimensionless coefficients that serve as coordinates; because the metric integrands depend only on $x$ and the fixed band edges, the metric is constant across parameter space. Eigen-decomposition of this metric, followed by a principal component analysis, reduces the placement problem to three dimensions, where an $A^*_3$ lattice with minimal match 0.97 covers the physical range of masses, aligned spins, and eccentricities with about 4.78 million templates.

What would settle it

Generate a population of eccentric BNS/NSBH injections with a waveform model that includes eccentricity-induced higher harmonics and spin–eccentricity couplings, or with $e_0>0.2$ at 15 Hz, and compute the fitting factor of the paper's 4.78-million-template bank; if the fraction of injections with FF$<0.97$ substantially exceeds 6% while the quasi-circular bank's loss remains comparable, the claim that the eccentric bank is highly effectual in the stated regime fails.

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Extended reading notes

Core claim

The central discovery is that the TaylorF2Ecc phase can be reparametrized by dimensionless coefficients of a frequency parameter $x=f/f_0$, and that in this coefficient space the matched-filter metric is constant (flat) over the whole BNS/NSBH parameter range. Projecting out the time axis, transforming to the eigenvectors of the metric, and keeping the first three principal components yields a three-dimensional Euclidean space in which mismatch equals squared distance. Placing an $A^*_3$ lattice in this space with a minimal match of 0.97 produces a bank of 4,781,475 templates. In Monte Carlo simulations against 60,000 eccentric TaylorF2Ecc injections, this bank has fitting factor above 0.95 for every injection and misses less than 6% of signals due to spacing, whereas a quasi-circular bank built on the same mass–spin space misses about 70% of the eccentric injections with FF$\le0.97$ and loses more than 40% of detection rate for the highest eccentricities. The authors also show, by setting the bank's template eccentricities to zero, that the gain comes from the new eccentricity dimension rather than from the larger bank size.

Load-bearing premise

The measured miss rates assume real eccentric BNS/NSBH signals are faithfully described by the inspiral-only, leading-order-eccentricity waveform TaylorF2Ecc; if actual signals carry stronger higher harmonics or spin–eccentricity phase terms, the bank's recovery rates and the comparison with quasi-circular banks could differ.

Editorial extensions

If this is right

  • Below an eccentricity of about $e_0\simeq0.03$ at 15 Hz, current quasi-circular banks are adequate, but above this value they increasingly miss signals, with more than 40% of the most eccentric BNS/NSBH systems lost.
  • The eccentric geometric bank keeps the detection-rate loss at a roughly constant level near 6% across the full eccentricity range, an order-of-magnitude improvement over the quasi-circular bank's 25–40% loss.
  • Because the improvement persists when comparing banks of similar template density, eccentricity itself—not the larger bank size—is the operative new search dimension.
  • The geometric placement keeps the eccentric bank only about 8.4 times larger than the quasi-circular one, making a dedicated eccentric search computationally feasible in the low-mass regime.
  • The eccentric bank also recovers quasi-circular BNS/NSBH signals nearly as well as a dedicated circular bank, so it can serve as a single unified search bank for this mass range.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A direct and testable extension is to run this bank on data from current ground-based detectors; the bank's coverage of aligned-spin BNS/NSBH mergers with $e_0$ up to 0.15 could reveal a population missed by circular-only pipelines.
  • The same flat-metric and principal-component construction could be extended to in-plane spins, higher eccentricity harmonics, or tidal effects, though each new physical effect would likely add principal components and increase the template count; the $e_0\simeq0.03$ threshold identifies when such effects start to matter.
  • The metric derived here could also accelerate parameter estimation for eccentric binaries, since a flat metric enables analytic or semi-analytic proposal distributions rather than expensive numerical exploration.
  • The reduction from five physical parameters to three significant principal components suggests a strong degeneracy structure in this mass and eccentricity range, which could inform reduced-order modelling of eccentric BNS/NSBH waveforms.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 6 minor

Summary. The paper presents a geometric template bank for aligned-spin, low-mass compact binaries (BNS and NSBH) with moderate orbital eccentricity, using the TaylorF2Ecc inspiral waveform. The authors reparametrize the waveform phase in terms of dimensionless PN coefficients, construct a globally flat metric in this coefficient space, apply PCA to obtain a three-dimensional effective metric space, and place an A*_3 lattice template bank with minimal match 0.97. They report that a quasi-circular TaylorF2 bank misses roughly 70% of eccentric injections with fitting factor below 0.97, corresponding to detection-rate losses exceeding 25% for e0>0.03 and reaching about 40% at the highest eccentricities considered, while their eccentric bank misses less than 6% of signals due to finite template spacing. The bank is about 8.4 times larger than the quasi-circular bank. A control experiment in which the eccentric templates are set to zero eccentricity shows that the improved recovery is due to the eccentric degree of freedom rather than the larger bank size.

Significance. If the reported performance carries over to real signals, the paper provides a substantial step toward including eccentricity in modelled matched-filter searches for BNS and NSBH binaries, a regime where current quasi-circular banks are known to be ineffectual. The strengths of the paper include: (i) a metric approximation validated against brute-force numerical matches with errors orders of magnitude below the minimal match (Figs. 1, 4, 5); (ii) a large injection study (60,000 injections per population) that accounts for selection effects via the effective fitting factor FFeff and includes a control bank to isolate the effect of eccentricity; (iii) a clear statement of the waveform-model limitations in Sec. VII. These are positive features that make the core methodology credible within the stated waveform family. However, the headline claims about detection rates are derived entirely from injections of the same simplified waveform model used to build the bank, and the paper does not yet quantify how those claims might change for more complete eccentric waveform models or for astrophysically motivated populations.

major comments (2)
  1. [Sec. VI, Table IV, Fig. 12; Eq. (13)] The central quantitative claims—that the eccentric bank misses less than 6% of signals and that the quasi-circular bank loses more than 25–40% of eccentric signals for e0>0.03—are obtained by injecting TaylorF2Ecc signals into banks built from the same TaylorF2Ecc phase expansion, with the eccentric phase truncated at 2PN (Eq. 13). The injections and templates are deliberately kept at the same PN orders (Sec. VI), so the measured miss rates quantify only discretization loss under the assumption that the 2PN-truncated TaylorF2Ecc is the true signal family. Real eccentric BNS/NSBH signals will contain eccentricity-induced higher harmonics, spin-eccentricity phase terms, and possibly the 3PN eccentric coefficients (kappa5, kappa6, kappa_l6) that are omitted here. The authors acknowledge these limitations qualitatively in Sec. VII, but the abstract and the conclusions in Sec. VI present the 6% and 25–40% numbers without this caveat. I request that the claims be explicitly qualified to the TaylorF2Ecc waveform family, or ideally that a subset of injections be repeated with a more complete eccentric waveform model (e.g., an EOB model) to quantify the systematic effect on the miss rates.
  2. [Sec. IV C and Sec. VI, Eq. (33)] The PCA basis used for the flat metric is derived from a uniform distribution over the physical parameter ranges in Table II, and the effective fitting factor FFeff in Eq. (33) is computed from injections drawn from the same uniform distribution. The reported detection-rate losses are therefore properties of this fiducial uniform population, not of an astrophysical population of eccentric BNS/NSBH binaries. The mass, spin, and eccentricity distributions of realistic populations could shift the loss rates, particularly for NSBH systems where the uniform mass prior may overweight asymmetric mass ratios. The paper should state this population dependence clearly and, if feasible, test the sensitivity of FFeff to alternative injection priors.
minor comments (6)
  1. [Appendix C, Eq. (C4)] The expression for kappa3 contains a term epsilon24 f^{31/9}_ecc, which appears to be a typo: at the f^{-25/9} power the 3PN contribution should involve epsilon33, and there is no epsilon34 coefficient defined in Appendix B. Please check this formula and correct it if it is indeed a typo.
  2. [Sec. VI and Table III] There is an inconsistency between the text and Table III for the injection sky and polarization distributions: the text states cos(theta) in U(0,1) and polarization angle in U(0,pi), while Table III lists cos(theta) in U(-1,1) and psi in U(0,2pi). Please harmonize these values.
  3. [Fig. 4] The y-axis label shows a fraction 'avg (|Mapx - Mnum|/Mnum)', while the text refers to 'average percentage error'; please make the axis label and the text consistent, and state whether the plotted quantity is a fraction or a percentage.
  4. [Sec. VI, first paragraph] The paper says the PN orders of injections and templates are kept the same, but it does not specify exactly which orders are used (e.g., 3.5PN quasi-circular phase and 2PN eccentric phase). Please state this explicitly for reproducibility.
  5. [Sec. IV B, Sec. VI, Fig. 1 caption] There are several typographical errors: 'and and f0' in Sec. IV B, 'litte' in Sec. VI, and 'thess ellipses' in the Fig. 1 caption. These should be corrected.
  6. [Eq. (30)] The notation 'n <= 12' in the sum is confusing because the bank uses only three principal components; please clarify that in practice the sum is truncated to the retained PCA components.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the bank's effectualness is measured by independent Monte Carlo fitting-factor simulations, and the flat metric is a self-contained coordinate transformation of the TaylorF2Ecc phase.

full rationale

The paper's central derivation—a globally flat metric from the TaylorF2Ecc phase coefficients, PCA dimensionality reduction, and A*_n lattice placement—is self-contained and is not used to claim detection efficiency by construction. The headline effectualness figures (≲6% missed by the eccentric bank; 25–40% loss for the quasi-circular bank) are obtained from explicit matched-filter bank simulations computing fitting factors against Monte Carlo injections, not from the metric or from posterior fits. The metric approximation is checked against numerical matches (Figs. 1, 4, 5), and the bank's improvement is controlled by setting template eccentricities to zero (Fig. 10), showing the gain is due to including eccentricity rather than bank size. Using TaylorF2Ecc for both injections and templates is a self-consistency test, and the paper explicitly acknowledges in Sec. VII that missing higher harmonics, spin-eccentricity coupling, and orbital-orientation effects limit the regime; this is a model-validity caveat, not circularity. Self-citations in the text are contextual (reviews, eccentricity-evolution references, waveform-model citations) and are not load-bearing for the construction or the measured performance. No fitted parameter is renamed as a prediction, no uniqueness theorem is imported from the authors' prior work, and no ansatz is smuggled in via citation. The paper's conclusions are model-dependent but not circular.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

The central claim rests on the chosen minimal match, frequency band, PCA truncation, and the waveform model TaylorF2Ecc. No astrophysical constants are fitted; the performance numbers come from Monte Carlo injections. The key domain assumption is that TaylorF2Ecc adequately represents real eccentric signals in the targeted regime.

free parameters (5)
  • Minimal match MM = 0.97
    Design target for template spacing; chosen a priori, affects bank size and the less than 6% miss rate.
  • Upper cutoff frequency fupper = 1000 Hz
    Choice for the metric calculation; tested over 300-1500 Hz with only small differences in match error; affects the metric and template density.
  • Number of PCA components = 3
    Selected based on average match error saturation (Fig. 4); used for lattice placement.
  • Inverse-mapping tolerance epsilon = 0.01
    Tolerance for finding physical parameters corresponding to lattice points; affects template placement accuracy.
  • PCA prior distribution = uniform over Table II ranges
    Used to compute the principal components; choice of prior affects the PCA basis.
assumptions (5)
  • standard math The overlap between nearby waveforms is well approximated by a second-order Taylor expansion (Fisher information metric).
    Standard in matched-filter template placement; invoked in Section IV A.
  • domain assumption The TaylorF2Ecc phase can be globally flattened by reparametrizing in terms of PN phase coefficients.
    Central to the method; tested numerically in Section IV C and Figs. 1-5.
  • domain assumption Detector noise is stationary and Gaussian, so the matched filter is optimal.
    Standard assumption for template-bank searches; stated in Section II.
  • domain assumption Three principal components capture the waveform variability across the parameter space.
    Validated by the error analysis in Fig. 4; the remaining components contribute mismatch less than 0.1.
  • standard math The A* lattice covering in 3D provides the specified minimal match for the flat metric.
    Standard lattice covering result used for template placement (Prix 2007).

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Cite this review

Pith. "Pith review of A geometric template bank for the detection of spinning low-mass compact binaries with moderate orbital eccentricity." pith.science (2026). https://pith.science/paper/EHRZFWK2

@misc{pith2026241206433,
  author       = {Pith},
  title        = {Pith review of: A geometric template bank for the detection of spinning low-mass compact binaries with moderate orbital eccentricity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EHRZFWK2}},
  note         = {Machine review of arXiv:2412.06433}
}
abstract

Compact binaries on eccentric orbits are another class of gravitational-wave (GW) sources that can provide a wealth of information on binary formation pathways and astrophysical environments. However, historically, eccentricity is often neglected in modelled GW searches for compact binaries. We show that currently used modelled searches that employ quasi-circular template banks are highly ineffectual in detecting binary neutron star (BNS) and neutron star--black hole (NSBH) systems with orbital eccentricities in the range of $[10^{-5},0.15]$ at a GW frequency of $15$Hz. For populations of moderately eccentric BNS and NSBH binaries with (anti-)aligned component spins, we demonstrate that quasi-circular template banks fail to detect up to $\sim 40\%$ of such systems. To alleviate these inefficiencies, we develop the first \emph{geometric} template bank for the search of BNSs and NSBH binaries that includes masses, (anti-)aligned spins and moderate eccentricity. Utilising the post-Newtonian inspiral waveform {\tt TaylorF2Ecc} and a global coordinate transformation, we construct a globally flat metric to efficiently place eccentric templates. Our geometric template bank is highly effectual, and significantly improves the recovery of eccentric signals with less than $6\%$ of signals missed due to the finite template spacing in the bank.

Figures

Figures reproduced from arXiv: 2412.06433 by the authors.

Figure 1
Figure 1. FIG. 1. Ambiguity ellipses on differences in [PITH_FULL_IMAGE:figures/full_fig_p008_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Block diagram showing the key steps for generat [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Depth or width of our targeted physical parameter [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Average error in the metric-based match M [PITH_FULL_IMAGE:figures/full_fig_p011_4.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Template density in hexagonal binning of different pairs of template parameters of the eccentric template bank. [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Visualisation of the eccentric template bank in the hexagonal binning of ( [PITH_FULL_IMAGE:figures/full_fig_p012_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8. Performance of the quasi-circular bank. [PITH_FULL_IMAGE:figures/full_fig_p015_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9. Performance of the eccentric bank. We show the [PITH_FULL_IMAGE:figures/full_fig_p015_9.png]
Figure 10
Figure 10. Figure 10: FIG. 10. Fitting factor of the eccentric bank, where the [PITH_FULL_IMAGE:figures/full_fig_p016_10.png]
Figure 11
Figure 11. Figure 11: FIG. 11. Impact of boundary effects [PITH_FULL_IMAGE:figures/full_fig_p017_11.png]
Figure 12
Figure 12. Figure 12: FIG. 12 [PITH_FULL_IMAGE:figures/full_fig_p017_12.png]

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Forward citations

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Reference graph

Works this paper leans on

211 extracted references · 11 canonical work pages · cited by 3 Pith papers

  1. [1]

    An aligned-spin, quasi-circular template bank gen- erated using a 3D A∗ n lattice

  2. [2]

    The bank simulations are performed using the workflow generator, pycbc make bank verifier workflow avail- able in PyCBC [193] with minor modifications in it

    An aligned-spin eccentric template bank generated using a 3D A∗ n lattice. The bank simulations are performed using the workflow generator, pycbc make bank verifier workflow avail- able in PyCBC [193] with minor modifications in it. A selection of figures of merit for our banks is presented in Table IV. As discussed before, there will inevitably be a diff...

  3. [3]

    Olsen, T

    S. Olsen, T. Venumadhav, J. Mushkin, J. Roulet, B. Za- ckay, and M. Zaldarriaga, New binary black hole merg- ers in the LIGO-Virgo O3a data, Phys. Rev. D 106, 043009 (2022), arXiv:2201.02252 [astro-ph.HE]

    arXiv 2022

  4. [4]

    Abbott et al

    R. Abbott et al. (KAGRA, VIRGO, LIGO Scientific), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the 22 Third Observing Run, Phys. Rev. X 13, 041039 (2023), arXiv:2111.03606 [gr-qc]

    arXiv 2023

  5. [5]

    A. H. Nitz, S. Kumar, Y.-F. Wang, S. Kastha, S. Wu, M. Sch¨ afer, R. Dhurkunde, and C. D. Capano, 4- OGC: Catalog of Gravitational Waves from Com- pact Binary Mergers, Astrophys. J. 946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]

    arXiv 2023

  6. [6]

    = Ψ′ QC(x;ζi,ζℓ i ) + Ψ′ Ecc(x :κi,κℓ 6) =−2ϕ0 +ζ0x−5/3 +ζ2x−1 +ζ3x−2/3 +ζ4x−1/3 +ζ6x1/3 +ζ7x2/3 +ζ8x +ζℓ 5 logx+ ζℓ 6 logxx 1/3 +κ0x−34/9 +κ2x−28/9 +κ3x−25/9 +κ4x−22/9 +κ5x−19/9 +κ6x−16/9+ κℓ 6 logxx−16/9. (C1) The dimensionless coefficients κi,κℓ i are given as κ0 = ( ε00f19/9 ecc +ε02f25/9 ecc +ε03f28/9 ecc +ε04f31/9 ecc ε05f34/9 ecc +ε06f37/9 ecc +εℓ ...

  7. [7]

    A. K. Mehta, S. Olsen, D. Wadekar, J. Roulet, T. Venu- madhav, J. Mushkin, B. Zackay, and M. Zaldarriaga, New binary black hole mergers in the LIGO-Virgo O3b data, (2023), arXiv:2311.06061 [gr-qc]

    arXiv 2023

  8. [8]

    Wadekar, J

    D. Wadekar, J. Roulet, T. Venumadhav, A. K. Mehta, B. Zackay, J. Mushkin, S. Olsen, and M. Zaldarriaga, New black hole mergers in the LIGO-Virgo O3 data from a gravitational wave search including higher-order harmonics, (2023), arXiv:2312.06631 [gr-qc]

    arXiv 2023

Show all 211 references
  1. [9]

    Aasi et al

    J. Aasi et al. (LIGO Scientific), Advanced LIGO, Class. Quant. Grav. 32, 074001 (2015), arXiv:1411.4547 [gr- qc]

    2015 arXiv

  2. [10]

    Acernese et al

    F. Acernese et al. (VIRGO), Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. Quant. Grav. 32, 024001 (2015), arXiv:1408.3978 [gr-qc]

    2015 arXiv

  3. [11]

    Y. Aso, Y. Michimura, K. Somiya, M. Ando, O. Miyakawa, T. Sekiguchi, D. Tatsumi, and H. Ya- mamoto (KAGRA), Interferometer design of the KA- GRA gravitational wave detector, Phys. Rev. D 88, 043007 (2013), arXiv:1306.6747 [gr-qc]

    2013 arXiv

  4. [12]

    Akutsu et al

    T. Akutsu et al. (KAGRA), Overview of KAGRA: De- tector design and construction history, PTEP 2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]

    2021

  5. [13]

    Abbott et al

    R. Abbott et al. (KAGRA, VIRGO, LIGO Scientific), Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3, Phys. Rev. X 13, 011048 (2023), arXiv:2111.03634 [astro-ph.HE]

    2023 arXiv

  6. [14]

    B. P. Abbott et al. (LIGO Scientific, Virgo), GW170817: Measurements of neutron star radii and equation of state, Phys. Rev. Lett. 121, 161101 (2018), arXiv:1805.11581 [gr-qc]

    2018 arXiv

  7. [15]

    B. P. Abbott et al. (LIGO Scientific, Virgo), Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant, Class. Quant. Grav. 37, 045006 (2020), arXiv:1908.01012 [gr-qc]

    2020 arXiv

  8. [16]

    Abbott et al

    R. Abbott et al. (LIGO Scientific, VIRGO, KAGRA), Tests of General Relativity with GWTC-3, (2021), arXiv:2112.06861 [gr-qc]

    2021 arXiv

  9. [17]

    Agazie et al

    G. Agazie et al. (NANOGrav), The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background, Astrophys. J. Lett. 951, L8 (2023), arXiv:2306.16213 [astro-ph.HE]

    2023 arXiv

  10. [18]

    Antoniadis et al

    J. Antoniadis et al. (EPTA), The second data release from the European Pulsar Timing Array III. Search for gravitational wave signals, Astron. Astrophys.678, A50 (2023), arXiv:2306.16214 [astro-ph.HE]

    2023 arXiv

  11. [19]

    D. J. Reardon et al. , Search for an Isotropic Gravitational-wave Background with the Parkes Pul- sar Timing Array, Astrophys. J. Lett. 951, L6 (2023), arXiv:2306.16215 [astro-ph.HE]

    2023 arXiv

  12. [20]

    Xu et al

    H. Xu et al. , Searching for the Nano-Hertz Stochas- tic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I, Res. Astron. As- trophys. 23, 075024 (2023), arXiv:2306.16216 [astro- ph.HE]

    2023 arXiv

  13. [21]

    S. A. Usman et al., The PyCBC search for gravitational waves from compact binary coalescence, Class. Quant. Grav. 33, 215004 (2016), arXiv:1508.02357 [gr-qc]

    2016 arXiv

  14. [22]

    A. H. Nitz, T. Dal Canton, D. Davis, and S. Reyes, Rapid detection of gravitational waves from compact binary mergers with PyCBC Live, Phys. Rev. D 98, 024050 (2018), arXiv:1805.11174 [gr-qc]

    2018 arXiv

  15. [23]

    Messick et al

    C. Messick et al. , Analysis Framework for the Prompt Discovery of Compact Binary Mergers in Gravitational-wave Data, Phys. Rev. D 95, 042001 (2017), arXiv:1604.04324 [astro-ph.IM]

    2017 arXiv

  16. [24]

    Aubin et al

    F. Aubin et al. , The MBTA pipeline for detecting com- pact binary coalescences in the third LIGO–Virgo ob- serving run, Class. Quant. Grav. 38, 095004 (2021), arXiv:2012.11512 [gr-qc]

    2021 arXiv

  17. [25]

    Chu et al

    Q. Chu et al. , SPIIR online coherent pipeline to search for gravitational waves from compact bi- nary coalescences, Phys. Rev. D 105, 024023 (2022), arXiv:2011.06787 [gr-qc]

    2022 arXiv

  18. [26]

    Venumadhav, B

    T. Venumadhav, B. Zackay, J. Roulet, L. Dai, and M. Zaldarriaga, New search pipeline for compact bi- nary mergers: Results for binary black holes in the first observing run of Advanced LIGO, Phys. Rev. D 100, 023011 (2019), arXiv:1902.10341 [astro-ph.IM]

    2019 arXiv

  19. [27]

    G. S. Davies, T. Dent, M. T´ apai, I. Harry, C. McIsaac, and A. H. Nitz, Extending the PyCBC search for gravitational waves from compact binary mergers to a global network, Phys. Rev. D 102, 022004 (2020), arXiv:2002.08291 [astro-ph.HE]

    2020 arXiv

  20. [28]

    Sachdev et al

    S. Sachdev et al. , The GstLAL Search Analysis Meth- ods for Compact Binary Mergers in Advanced LIGO’s Second and Advanced Virgo’s First Observing Runs, (2019), arXiv:1901.08580 [gr-qc]

    2019 arXiv

  21. [29]

    Dal Canton, A

    T. Dal Canton, A. H. Nitz, B. Gadre, G. S. Cabourn Davies, V. Villa-Ortega, T. Dent, I. Harry, and L. Xiao, Real-time Search for Compact Binary Merg- ers in Advanced LIGO and Virgo’s Third Observing Run Using PyCBC Live, Astrophys. J. 923, 254 (2021), arXiv:2008.07494 [astro-ph.HE]

    2021 arXiv

  22. [30]

    Wadekar, T

    D. Wadekar, T. Venumadhav, J. Roulet, A. K. Mehta, B. Zackay, J. Mushkin, and M. Zaldarriaga, New search pipeline for gravitational waves with higher-order modes using mode-by-mode filtering, Phys. Rev. D 110, 044063 (2024), arXiv:2405.17400 [gr-qc]

    2024 arXiv

  23. [31]

    B. S. Sathyaprakash and S. V. Dhurandhar, Choice of filters for the detection of gravitational waves from co- alescing binaries, Phys. Rev. D 44, 3819 (1991)

    1991

  24. [32]

    S. V. Dhurandhar and B. S. Sathyaprakash, Choice of filters for the detection of gravitational waves from co- alescing binaries. 2. Detection in colored noise, Phys. Rev. D 49, 1707 (1994)

    1994

  25. [33]

    B. J. Owen and B. S. Sathyaprakash, Matched filter- ing of gravitational waves from inspiraling compact bi- naries: Computational cost and template placement, Phys. Rev. D 60, 022002 (1999), arXiv:gr-qc/9808076

    1999 arXiv

  26. [34]

    Allen, W

    B. Allen, W. G. Anderson, P. R. Brady, D. A. Brown, and J. D. E. Creighton, FINDCHIRP: An Algorithm for detection of gravitational waves from inspiraling com- pact binaries, Phys. Rev. D85, 122006 (2012), arXiv:gr- qc/0509116. 23

    2012

  27. [35]

    Schmidt, Gravitational Waves From Binary Black Hole Mergers: Modeling and Observations, Front

    P. Schmidt, Gravitational Waves From Binary Black Hole Mergers: Modeling and Observations, Front. As- tron. Space Sci. 7, 28 (2020)

    2020

  28. [36]

    T. A. Apostolatos, C. Cutler, G. J. Sussman, and K. S. Thorne, Spin induced orbital precession and its mod- ulation of the gravitational wave forms from merging binaries, Phys. Rev. D 49, 6274 (1994)

    1994

  29. [37]

    L. E. Kidder, Coalescing binary systems of compact ob- jects to postNewtonian 5/2 order. 5. Spin effects, Phys. Rev. D 52, 821 (1995), arXiv:gr-qc/9506022

    1995 arXiv

  30. [38]

    Schmidt, M

    P. Schmidt, M. Hannam, S. Husa, and P. Ajith, Tracking the precession of compact binaries from their gravitational-wave signal, Phys. Rev. D 84, 024046 (2011), arXiv:1012.2879 [gr-qc]

    2011 arXiv

  31. [39]

    Y. Pan, A. Buonanno, M. Boyle, L. T. Buchman, L. E. Kidder, H. P. Pfeiffer, and M. A. Scheel, Inspiral- merger-ringdown multipolar waveforms of nonspinning black-hole binaries using the effective-one-body formal- ism, Phys. Rev. D 84, 124052 (2011), arXiv:1106.1021 [gr-qc]

    2011 arXiv

  32. [40]

    P. C. Peters and J. Mathews, Gravitational radiation from point masses in a Keplerian orbit, Phys. Rev. 131, 435 (1963)

    1963

  33. [41]

    Skliris, M

    V. Skliris, M. R. K. Norman, and P. J. Sutton, Real-Time Detection of Unmodelled Gravitational- Wave Transients Using Convolutional Neural Networks, (2020), arXiv:2009.14611 [astro-ph.IM]

    2020

  34. [42]

    Klimenko, I

    S. Klimenko, I. Yakushin, A. Mercer, and G. Mitsel- makher, Coherent method for detection of gravitational wave bursts, Class. Quant. Grav. 25, 114029 (2008), arXiv:0802.3232 [gr-qc]

    2008 arXiv

  35. [43]

    Lynch, S

    R. Lynch, S. Vitale, R. Essick, E. Katsavounidis, and F. Robinet, Information-theoretic approach to the gravitational-wave burst detection problem, Phys. Rev. D 95, 104046 (2017), arXiv:1511.05955 [gr-qc]

    2017 arXiv

  36. [44]

    A. G. Abac et al. (LIGO Scientific, KAGRA, VIRGO), Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo, Astrophys. J. 973, 132 (2024), arXiv:2308.03822 [astro-ph.HE]

    2024 arXiv

  37. [45]

    Van Den Broeck, D

    C. Van Den Broeck, D. A. Brown, T. Cokelaer, I. Harry, G. Jones, B. S. Sathyaprakash, H. Tagoshi, and H. Taka- hashi, Template banks to search for compact binaries with spinning components in gravitational wave data, Phys. Rev. D 80, 024009 (2009), arXiv:0904.1715 [gr- qc]

    2009 arXiv

  38. [46]

    Harry, S

    I. Harry, S. Privitera, A. Boh´ e, and A. Buonanno, Searching for Gravitational Waves from Compact Bi- naries with Precessing Spins, Phys. Rev. D 94, 024012 (2016), arXiv:1603.02444 [gr-qc]

    2016 arXiv

  39. [47]

    McIsaac, C

    C. McIsaac, C. Hoy, and I. Harry, Search technique to observe precessing compact binary mergers in the ad- vanced detector era, Phys. Rev. D 108, 123016 (2023), arXiv:2303.17364 [gr-qc]

    2023 arXiv

  40. [48]

    Schmidt et al

    S. Schmidt et al. , Searching for gravitational-wave signals from precessing black hole binaries with the GstLAL pipeline, Phys. Rev. D 110, 023038 (2024), arXiv:2403.17186 [gr-qc]

    2024 arXiv

  41. [49]

    A. H. Nitz and Y.-F. Wang, Search for gravitational waves from the coalescence of sub-solar mass and ec- centric compact binaries, The Astrophysical Journal 10.3847/1538-4357/ac01d9 (2021), arXiv:2102.00868 [astro-ph.HE]

    2021 arXiv

  42. [50]

    S. Schmidt et al., Searching for asymmetric and heavily precessing Binary Black Holes in the gravitational wave data from the LIGO and Virgo third Observing Run, (2024), arXiv:2406.17832 [gr-qc]

    2024 arXiv

  43. [51]

    Dhurkunde and A

    R. Dhurkunde and A. H. Nitz, Search for eccentric NSBH and BNS mergers in the third observing run of Advanced LIGO and Virgo, (2023), arXiv:2311.00242 [astro-ph.HE]

    2023 arXiv

  44. [52]

    A. K. Lenon, D. A. Brown, and A. H. Nitz, Eccentric bi- nary neutron star search prospects for Cosmic Explorer, Phys. Rev. D 104, 063011 (2021), arXiv:2103.14088 [astro-ph.HE]

    2021 arXiv

  45. [53]

    P. C. Peters, Gravitational Radiation and the Motion of Two Point Masses, Phys. Rev. 136, B1224 (1964)

    1964

  46. [54]

    C. S. Ye, W.-f. Fong, K. Kremer, C. L. Rodriguez, S. Chatterjee, G. Fragione, and F. A. Rasio, On the Rate of Neutron Star Binary Mergers from Globular Clusters, Astrophys. J. Lett. 888, L10 (2020), arXiv:1910.10740 [astro-ph.HE]

    2020 arXiv

  47. [55]

    Samsing, Eccentric Black Hole Mergers Forming in Globular Clusters, Phys

    J. Samsing, Eccentric Black Hole Mergers Forming in Globular Clusters, Phys. Rev. D 97, 103014 (2018), arXiv:1711.07452 [astro-ph.HE]

    2018 arXiv

  48. [56]

    C. L. Rodriguez, P. Amaro-Seoane, S. Chatterjee, K. Kremer, F. A. Rasio, J. Samsing, C. S. Ye, and M. Zevin, Post-Newtonian Dynamics in Dense Star Clusters: Formation, Masses, and Merger Rates of Highly-Eccentric Black Hole Binaries, Phys. Rev. D 98, 123005 (2018), arXiv:1811....

    2018 arXiv

  49. [57]

    Zevin, I

    M. Zevin, I. M. Romero-Shaw, K. Kremer, E. Thrane, and P. D. Lasky, Implications of Eccentric Observa- tions on Binary Black Hole Formation Channels, Astro- phys. J. Lett. 921, L43 (2021), arXiv:2106.09042 [astro- ph.HE]

    2021 arXiv

  50. [58]

    Yang, R.-G

    T. Yang, R.-G. Cai, Z. Cao, and H. M. Lee, Eccentric- ity of Long Inspiraling Compact Binaries Sheds Light on Dark Sirens, Phys. Rev. Lett. 129, 191102 (2022), arXiv:2202.08608 [gr-qc]

    2022 arXiv

  51. [59]

    B. Sun, Z. Cao, Y. Wang, and H.-C. Yeh, Parameter estimation of eccentric inspiraling compact binaries us- ing an enhanced post circular model for ground-based detectors, Phys. Rev. D 92, 044034 (2015)

    2015

  52. [60]

    Z. Xuan, S. Naoz, and X. Chen, Detecting accelerating eccentric binaries in the LISA band, Phys. Rev. D 107, 043009 (2023), arXiv:2210.03129 [astro-ph.HE]

    2023 arXiv

  53. [61]

    Favata, Systematic parameter errors in inspiraling neutron star binaries, Phys

    M. Favata, Systematic parameter errors in inspiraling neutron star binaries, Phys. Rev. Lett. 112, 101101 (2014), arXiv:1310.8288 [gr-qc]

    2014 arXiv

  54. [62]

    Narayan, N

    P. Narayan, N. K. Johnson-McDaniel, and A. Gupta, Effect of ignoring eccentricity in testing general relativ- ity with gravitational waves, Phys. Rev. D 108, 064003 (2023), arXiv:2306.04068 [gr-qc]

    2023 arXiv

  55. [63]

    Saini, M

    P. Saini, M. Favata, and K. G. Arun, Systematic bias on parametrized tests of general relativity due to neglect of orbital eccentricity, Phys. Rev. D 106, 084031 (2022), arXiv:2203.04634 [gr-qc]

    2022 arXiv

  56. [64]

    Dutta Roy and P

    P. Dutta Roy and P. Saini, Impact of unmodeled eccen- tricity on the tidal deformability measurement and im- plications for gravitational wave physics inference, Phys. Rev. D 110, 024002 (2024), arXiv:2403.02404 [astro- ph.HE]

    2024 arXiv

  57. [65]

    M. A. Shaikh, S. A. Bhat, and S. J. Kapadia, A study of the inspiral-merger-ringdown consistency test with gravitational-wave signals from compact binaries in eccentric orbits, Phys. Rev. D 110, 024030 (2024), arXiv:2402.15110 [gr-qc]

    2024 arXiv

  58. [66]

    I. M. Romero-Shaw, P. D. Lasky, and E. Thrane, Signs 24 of Eccentricity in Two Gravitational-wave Signals May Indicate a Subpopulation of Dynamically Assembled Bi- nary Black Holes, Astrophys. J. Lett. 921, L31 (2021), arXiv:2108.01284 [astro-ph.HE]

    2021 arXiv

  59. [67]

    I. M. Romero-Shaw, P. D. Lasky, and E. Thrane, Four Eccentric Mergers Increase the Evidence that LIGO–Virgo–KAGRA’s Binary Black Holes Form Dynamically, Astrophys. J. 940, 171 (2022), arXiv:2206.14695 [astro-ph.HE]

    2022 arXiv

  60. [68]

    O’Shea and P

    E. O’Shea and P. Kumar, Correlations in gravitational- wave reconstructions from eccentric binaries: A case study with GW151226 and GW170608, Phys. Rev. D 108, 104018 (2023), arXiv:2107.07981 [astro-ph.HE]

    2023 arXiv

  61. [69]

    Gupte et al

    N. Gupte et al. , Evidence for eccentricity in the pop- ulation of binary black holes observed by LIGO-Virgo- KAGRA, (2024), arXiv:2404.14286 [gr-qc]

    2024 arXiv

  62. [70]

    H. L. Iglesias et al. , Eccentricity Estimation for Five Binary Black Hole Mergers with Higher-order Gravitational-wave Modes, Astrophys. J. 972, 65 (2024), arXiv:2208.01766 [gr-qc]

    2024 arXiv

  63. [71]

    Ramos-Buades, A

    A. Ramos-Buades, A. Buonanno, and J. Gair, Bayesian inference of binary black holes with inspiral-merger- ringdown waveforms using two eccentric parameters, Phys. Rev. D 108, 124063 (2023), arXiv:2309.15528 [gr- qc]

    2023 arXiv

  64. [72]

    Gayathri, J

    V. Gayathri, J. Healy, J. Lange, B. O’Brien, M. Szczep- anczyk, I. Bartos, M. Campanelli, S. Klimenko, C. O. Lousto, and R. O’Shaughnessy, Eccentricity estimate for black hole mergers with numerical relativity simula- tions, Nature Astron. 6, 344 (2022), arXiv:2009.05461 [astro-ph.HE]

    2022 arXiv

  65. [73]

    S. Wu, Z. Cao, and Z.-H. Zhu, Measuring the eccen- tricity of binary black holes in GWTC-1 by using the inspiral-only waveform, Mon. Not. Roy. Astron. Soc. 495, 466 (2020), arXiv:2002.05528 [astro-ph.IM]

    2020 arXiv

  66. [74]

    Gamba, M

    R. Gamba, M. Breschi, G. Carullo, S. Albanesi, P. Ret- tegno, S. Bernuzzi, and A. Nagar, GW190521 as a dy- namical capture of two nonspinning black holes, Nature Astron. 7, 11 (2023), arXiv:2106.05575 [gr-qc]

    2023 arXiv

  67. [75]

    Bonino, R

    A. Bonino, R. Gamba, P. Schmidt, A. Nagar, G. Prat- ten, M. Breschi, P. Rettegno, and S. Bernuzzi, Inferring eccentricity evolution from observations of coalescing binary black holes, Phys. Rev. D 107, 064024 (2023), arXiv:2207.10474 [gr-qc]

    2023 arXiv

  68. [76]

    D. A. Brown and P. J. Zimmerman, The Effect of Ec- centricity on Searches for Gravitational-Waves from Co- alescing Compact Binaries in Ground-based Detectors, Phys. Rev. D 81, 024007 (2010), arXiv:0909.0066 [gr- qc]

    2010 arXiv

  69. [77]

    Cokelaer and D

    T. Cokelaer and D. Pathak, Searching for gravitational- wave signals emitted by eccentric compact binaries us- ing a non-eccentric template bank: Implications for ground-based detectors, Class. Quant. Grav.26, 045013 (2009), arXiv:0903.4791 [gr-qc]

    2009 arXiv

  70. [78]

    E. A. Huerta and D. A. Brown, Effect of eccentricity on binary neutron star searches in Advanced LIGO, Phys. Rev. D 87, 127501 (2013), arXiv:1301.1895 [gr-qc]

    2013 arXiv

  71. [79]

    Wang and A

    Y.-F. Wang and A. H. Nitz, Prospects for de- tecting gravitational waves from eccentric subsolar mass compact binaries, Astrophys. J. 912, 53 (2021), arXiv:2101.12269 [astro-ph.HE]

    2021 arXiv

  72. [80]

    Kumar, S

    Divyajyoti, S. Kumar, S. Tibrewal, I. M. Romero-Shaw, and C. K. Mishra, Blind spots and biases: The dan- gers of ignoring eccentricity in gravitational-wave sig- nals from binary black holes, Phys. Rev. D 109, 043037 (2024), arXiv:2309.16638 [gr-qc]

    2024 arXiv

  73. [81]

    Gadre, K

    B. Gadre, K. Soni, S. Tiwari, A. Ramos-Buades, M. Haney, and S. Mitra, Detectability of eccentric bi- nary black holes with matched filtering and unmod- eled pipelines during the third observing run of LIGO- Virgo-KAGRA, Phys. Rev. D 110, 044013 (2024), arXiv:2405.04186 [gr-qc]

    2024 arXiv

  74. [82]

    Ramos-Buades, S

    A. Ramos-Buades, S. Tiwari, M. Haney, and S. Husa, Impact of eccentricity on the gravitational wave searches for binary black holes: High mass case, Phys. Rev. D 102, 043005 (2020), arXiv:2005.14016 [gr-qc]

    2020 arXiv

  75. [83]

    A. H. Nitz, A. Lenon, and D. A. Brown, Search for Ec- centric Binary Neutron Star Mergers in the first and second observing runs of Advanced LIGO, Astrophys. J. 890, 1 (2019), arXiv:1912.05464 [astro-ph.HE]

    2019 arXiv

  76. [84]

    A. H. Nitz and Y.-F. Wang, Search for Gravitational Waves from the Coalescence of Subsolar-Mass Binaries in the First Half of Advanced LIGO and Virgo’s Third Observing Run, Phys. Rev. Lett. 127, 151101 (2021), arXiv:2106.08979 [astro-ph.HE]

    2021 arXiv

  77. [85]

    A. H. Nitz and Y.-F. Wang, Broad search for gravita- tional waves from subsolar-mass binaries through LIGO and Virgo’s third observing run, Phys. Rev. D 106, 023024 (2022), arXiv:2202.11024 [astro-ph.HE]

    2022 arXiv

  78. [86]

    Kacanja, A

    K. Kacanja, A. H. Nitz, S. Wu, M. Cusinato, R. Dhurkunde, I. Harry, T. Dal Canton, and F. Pan- narale, Efficient Stochastic Template Bank using Inner Product Inequalities, (2024), arXiv:2407.03406 [astro- ph.HE]

    2024 arXiv

  79. [87]

    Pal and K

    S. Pal and K. R. Nayak, Swarm-intelligent search for gravitational waves from eccentric binary mergers, Phys. Rev. D 110, 042003 (2024), arXiv:2307.03736 [gr- qc]

    2024 arXiv

  80. [88]

    Tiwari et al

    V. Tiwari et al. , Proposed search for the detection of gravitational waves from eccentric binary black holes, Phys. Rev. D 93, 043007 (2016), arXiv:1511.09240 [gr- qc]

    2016 arXiv

  81. [89]

    B. P. Abbott et al. (LIGO Scientific, Virgo), Search for Eccentric Binary Black Hole Mergers with Advanced LIGO and Advanced Virgo during their First and Sec- ond Observing Runs, Astrophys. J. 883, 149 (2019), arXiv:1907.09384 [astro-ph.HE]

    2019 arXiv

  82. [90]

    Abbott et al

    R. Abbott et al. (KAGRA, VIRGO, LIGO Scien- tific), All-sky search for long-duration gravitational- wave bursts in the third Advanced LIGO and Ad- vanced Virgo run, Phys. Rev. D 104, 102001 (2021), arXiv:2107.13796 [gr-qc]

    2021 arXiv

  83. [91]

    Moore, M

    B. Moore, M. Favata, K. G. Arun, and C. K. Mishra, Gravitational-wave phasing for low-eccentricity inspi- ralling compact binaries to 3PN order, Phys. Rev. D 93, 124061 (2016), arXiv:1605.00304 [gr-qc]

    2016 arXiv

  84. [92]

    Ramos-Buades, A

    A. Ramos-Buades, A. Buonanno, H. Estell´ es, M. Khalil, D. P. Mihaylov, S. Ossokine, L. Pompili, and M. Shiferaw, Next generation of accurate and ef- ficient multipolar precessing-spin effective-one-body waveforms for binary black holes, Phys. Rev. D 108, 124037 (2023), arXiv:...

    2023 arXiv

  85. [93]

    Pratten et al

    G. Pratten et al. , Computationally efficient models for the dominant and subdominant harmonic modes of pre- cessing binary black holes, Phys. Rev. D 103, 104056 (2021), arXiv:2004.06503 [gr-qc]

    2021 arXiv

  86. [94]

    Adams, D

    T. Adams, D. Buskulic, V. Germain, G. M. Guidi, F. Marion, M. Montani, B. Mours, F. Piergiovanni, and 25 G. Wang, Low-latency analysis pipeline for compact bi- nary coalescences in the advanced gravitational wave detector era, Class. Quant. Grav. 33, 175012 (2016), arXiv:1512....

    2016 arXiv

  87. [95]

    Abbott et al

    R. Abbott et al. (LIGO Scientific, Virgo), Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo, SoftwareX 13, 100658 (2021), arXiv:1912.11716 [gr-qc]

    2021 arXiv

  88. [96]

    Abbott et al

    R. Abbott et al. (KAGRA, VIRGO, LIGO Scientific), Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO, Astrophys. J. Suppl. 267, 29 (2023), arXiv:2302.03676 [gr-qc]

    2023 arXiv

  89. [97]

    Wiener, Extrapolation, Interpolation, and Smoothing of Stationary Time Series: With Engineering Applica- tions (MIT Press, Cambridge, MA, 1949)

    N. Wiener, Extrapolation, Interpolation, and Smoothing of Stationary Time Series: With Engineering Applica- tions (MIT Press, Cambridge, MA, 1949)

    1949

  90. [98]

    Wang and S

    Y. Wang and S. D. Mohanty, Particle Swarm Optimiza- tion and gravitational wave data analysis: Performance on a binary inspiral testbed, Phys. Rev. D 81, 063002 (2010), arXiv:1001.0923 [gr-qc]

    2010 arXiv

  91. [99]

    M. E. Normandin and S. D. Mohanty, Towards a real-time fully-coherent all-sky search for gravitational waves from compact binary coalescences using particle swarm optimization, Phys. Rev. D 101, 082001 (2020), arXiv:2002.02150 [astro-ph.IM]

    2020 arXiv

  92. [100]

    Srivastava, K

    V. Srivastava, K. Rajesh Nayak, and S. Bose, Toward low-latency coincident precessing and coherent aligned- spin gravitational-wave searches of compact binary co- alescences with particle swarm optimization, (2018), arXiv:1811.02401 [astro-ph.IM]

    2018 arXiv

  93. [101]

    Allen, χ2 time-frequency discriminator for gravita- tional wave detection, Phys

    B. Allen, χ2 time-frequency discriminator for gravita- tional wave detection, Phys. Rev. D 71, 062001 (2005), arXiv:gr-qc/0405045

    2005 arXiv

  94. [102]

    A. H. Nitz, Distinguishing short duration noise tran- sients in LIGO data to improve the PyCBC search for gravitational waves from high mass binary black hole mergers, Class. Quant. Grav. 35, 035016 (2018), arXiv:1709.08974 [gr-qc]

    2018 arXiv

  95. [103]

    McIsaac and I

    C. McIsaac and I. Harry, Using machine learning to au- totune chi-squared tests for gravitational wave searches, Phys. Rev. D 105, 104056 (2022), arXiv:2203.03449 [gr- qc]

    2022 arXiv

  96. [104]

    Schmidt and S

    S. Schmidt and S. Caudill, Novel signal-consistency test for gravitational-wave searches of generic black hole binaries, Phys. Rev. D 110, 023042 (2024), arXiv:2403.17179 [gr-qc]

    2024 arXiv

  97. [105]

    G. M. Manca and M. Vallisneri, Cover art: Issues in the metric-guided and metric-less placement of random and stochastic template banks, Phys. Rev. D81, 024004 (2010), arXiv:0909.0563 [gr-qc]

    2010 arXiv

  98. [106]

    Allen, Optimal template banks, Phys

    B. Allen, Optimal template banks, Phys. Rev. D 104, 042005 (2021), arXiv:2102.11254 [astro-ph.IM]

    2021 arXiv

  99. [107]

    Babak, R

    S. Babak, R. Balasubramanian, D. Churches, T. Coke- laer, and B. S. Sathyaprakash, A Template bank to search for gravitational waves from inspiralling compact binaries. I. Physical models, Class. Quant. Grav. 23, 5477 (2006), arXiv:gr-qc/0604037

    2006 arXiv

  100. [108]

    Cokelaer, Gravitational waves from inspiralling com- pact binaries: Hexagonal template placement and its efficiency in detecting physical signals, Phys

    T. Cokelaer, Gravitational waves from inspiralling com- pact binaries: Hexagonal template placement and its efficiency in detecting physical signals, Phys. Rev. D 76, 102004 (2007), arXiv:0706.4437 [gr-qc]

    2007 arXiv

  101. [109]

    D. A. Brown, I. Harry, A. Lundgren, and A. H. Nitz, Detecting binary neutron star systems with spin in ad- vanced gravitational-wave detectors, Phys. Rev. D 86, 084017 (2012), arXiv:1207.6406 [gr-qc]

    2012 arXiv

  102. [110]

    I. W. Harry, A. H. Nitz, D. A. Brown, A. P. Lundgren, E. Ochsner, and D. Keppel, Investigating the effect of precession on searches for neutron-star-black-hole bina- ries with Advanced LIGO, Phys. Rev. D 89, 024010 (2014), arXiv:1307.3562 [gr-qc]

    2014 arXiv

  103. [111]

    Roulet, L

    J. Roulet, L. Dai, T. Venumadhav, B. Zackay, and M. Zaldarriaga, Template Bank for Compact Binary Coalescence Searches in Gravitational Wave Data: A General Geometric Placement Algorithm, Phys. Rev. D 99, 123022 (2019), arXiv:1904.01683 [astro-ph.IM]

    2019 arXiv

  104. [112]

    Babak, Building a stochastic template bank for de- tecting massive black hole binaries, Class

    S. Babak, Building a stochastic template bank for de- tecting massive black hole binaries, Class. Quant. Grav. 25, 195011 (2008), arXiv:0801.4070 [gr-qc]

    2008 arXiv

  105. [113]

    I. W. Harry, B. Allen, and B. S. Sathyaprakash, A Stochastic template placement algorithm for gravita- tional wave data analysis, Phys. Rev. D 80, 104014 (2009), arXiv:0908.2090 [gr-qc]

    2009 arXiv

  106. [114]

    Ajith, N

    P. Ajith, N. Fotopoulos, S. Privitera, A. Neunzert, and A. J. Weinstein, Effectual template bank for the de- tection of gravitational waves from inspiralling compact binaries with generic spins, Phys. Rev. D 89, 084041 (2014), arXiv:1210.6666 [gr-qc]

    2014 arXiv

  107. [115]

    Privitera, S

    S. Privitera, S. R. P. Mohapatra, P. Ajith, K. Can- non, N. Fotopoulos, M. A. Frei, C. Hanna, A. J. Wein- stein, and J. T. Whelan, Improving the sensitivity of a search for coalescing binary black holes with nonprecess- ing spins in gravitational wave data, Phys. Rev. D 89, 02...

    2014 arXiv

  108. [116]

    Fehrmann and H

    H. Fehrmann and H. J. Pletsch, Efficient generation and optimization of stochastic template banks by a neigh- boring cell algorithm, Phys. Rev. D 90, 124049 (2014), arXiv:1411.3899 [astro-ph.IM]

    2014 arXiv

  109. [117]

    S. Roy, A. S. Sengupta, and P. Ajith, Effectual tem- plate banks for upcoming compact binary searches in Advanced-LIGO and Virgo data, Phys. Rev. D 99, 024048 (2019), arXiv:1711.08743 [gr-qc]

    2019 arXiv

  110. [118]

    S. Roy, A. S. Sengupta, and N. Thakor, Hy- brid geometric-random template-placement algorithm for gravitational wave searches from compact bi- nary coalescences, Phys. Rev. D 95, 104045 (2017), arXiv:1702.06771 [gr-qc]

    2017 arXiv

  111. [119]

    Sharma, S

    A. Sharma, S. Roy, and A. S. Sengupta, Template bank to search for exotic gravitational wave signals from as- trophysical compact binaries, Phys. Rev. D109, 124049 (2024), arXiv:2311.03274 [gr-qc]

    2024 arXiv

  112. [120]

    Messenger, R

    C. Messenger, R. Prix, and M. A. Papa, Random tem- plate banks and relaxed lattice coverings, Phys. Rev. D 79, 104017 (2009), arXiv:0809.5223 [gr-qc]

    2009 arXiv

  113. [121]

    Rover, Random template placement and prior in- formation, J

    C. Rover, Random template placement and prior in- formation, J. Phys. Conf. Ser. 228, 012008 (2010), arXiv:0911.5051 [gr-qc]

    2010 arXiv

  114. [122]

    Coogan, T

    A. Coogan, T. D. P. Edwards, H. S. Chia, R. N. George, K. Freese, C. Messick, C. N. Setzer, C. Weniger, and A. Zimmerman, Efficient gravitational wave template bank generation with differentiable waveforms, Phys. Rev. D 106, 122001 (2022), arXiv:2202.09380 [astro- ph.IM]

    2022 arXiv

  115. [123]

    Schmidt, B

    S. Schmidt, B. Gadre, and S. Caudill, Gravitational- wave template banks for novel compact binaries, Phys. Rev. D 109, 042005 (2024), arXiv:2302.00436 [gr-qc]

    2024 arXiv

  116. [124]

    Prix, Template-based searches for gravitational waves: Efficient lattice covering of flat parame- ter spaces, Class

    R. Prix, Template-based searches for gravitational waves: Efficient lattice covering of flat parame- ter spaces, Class. Quant. Grav. 24, S481 (2007), arXiv:0707.0428 [gr-qc]. 26

    2007 arXiv

  117. [125]

    Babak et al

    S. Babak et al. , Searching for gravitational waves from binary coalescence, Phys. Rev. D 87, 024033 (2013), arXiv:1208.3491 [gr-qc]

    2013 arXiv

  118. [126]

    Balasubramanian, B

    R. Balasubramanian, B. S. Sathyaprakash, and S. V. Dhurandhar, Gravitational waves from coalescing bina- ries: Detection strategies and Monte Carlo estimation of parameters, Phys. Rev. D 53, 3033 (1996), [Erratum: Phys.Rev.D 54, 1860 (1996)], arXiv:gr-qc/9508011

    1996 arXiv

  119. [127]

    Indik, H

    N. Indik, H. Fehrmann, F. Harke, B. Krishnan, and A. B. Nielsen, Reducing the number of templates for aligned-spin compact binary coalescence gravitational wave searches using metric-agnostic template nudging, Phys. Rev. D 97, 124008 (2018), arXiv:1712.07869 [gr- qc]

    2018 arXiv

  120. [128]

    Capano, I

    C. Capano, I. Harry, S. Privitera, and A. Buonanno, Implementing a search for gravitational waves from bi- nary black holes with nonprecessing spin, Phys. Rev. D 93, 124007 (2016), arXiv:1602.03509 [gr-qc]

    2016 arXiv

  121. [129]

    Dal Canton and I

    T. Dal Canton and I. W. Harry, Designing a tem- plate bank to observe compact binary coalescences in Advanced LIGO’s second observing run, (2017), arXiv:1705.01845 [gr-qc]

    2017 arXiv

  122. [130]

    Moore and N

    B. Moore and N. Yunes, A 3PN Fourier Domain Waveform for Non-Spinning Binaries with Moderate Eccentricity, Class. Quant. Grav. 36, 185003 (2019), arXiv:1903.05203 [gr-qc]

    2019 arXiv

  123. [131]

    Tiwari, G

    S. Tiwari, G. Achamveedu, M. Haney, and P. He- mantakumar, Ready-to-use Fourier domain templates for compact binaries inspiraling along moderately ec- centric orbits, Phys. Rev. D 99, 124008 (2019), arXiv:1905.07956 [gr-qc]

    2019 arXiv

  124. [132]

    Tanay, M

    S. Tanay, M. Haney, and A. Gopakumar, Frequency and time domain inspiral templates for comparable mass compact binaries in eccentric orbits, Phys. Rev. D 93, 064031 (2016), arXiv:1602.03081 [gr-qc]

    2016 arXiv

  125. [133]

    E. A. Huerta, P. Kumar, S. T. McWilliams, R. O’Shaughnessy, and N. Yunes, Accurate and effi- cient waveforms for compact binaries on eccentric or- bits, Phys. Rev. D 90, 084016 (2014), arXiv:1408.3406 [gr-qc]

    2014 arXiv

  126. [134]

    Klein, Y

    A. Klein, Y. Boetzel, A. Gopakumar, P. Jetzer, and L. de Vittori, Fourier domain gravitational waveforms for precessing eccentric binaries, Phys. Rev. D 98, 104043 (2018), arXiv:1801.08542 [gr-qc]

    2018 arXiv

  127. [135]

    Klein, EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals, (2021), arXiv:2106.10291 [gr-qc]

    A. Klein, EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals, (2021), arXiv:2106.10291 [gr-qc]

    2021 arXiv

  128. [136]

    J. N. Arredondo, A. Klein, and N. Yunes, Efficient gravitational-wave model for fully-precessing and mod- erately eccentric, compact binary inspirals, Phys. Rev. D 110, 044044 (2024), arXiv:2402.06804 [gr-qc]

    2024 arXiv

  129. [137]

    Blanchet, Gravitational Radiation from Post- Newtonian Sources and Inspiralling Compact Binaries, Living Rev

    L. Blanchet, Gravitational Radiation from Post- Newtonian Sources and Inspiralling Compact Binaries, Living Rev. Rel. 17, 2 (2014), arXiv:1310.1528 [gr-qc]

    2014 arXiv

  130. [138]

    Islam, V

    T. Islam, V. Varma, J. Lodman, S. E. Field, G. Khanna, M. A. Scheel, H. P. Pfeiffer, D. Gerosa, and L. E. Kid- der, Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: compa- rable mass, nonspinning case, Phys. Rev. D103, 064022 ...

    2021 arXiv

  131. [139]

    Buonanno and T

    A. Buonanno and T. Damour, Effective one-body ap- proach to general relativistic two-body dynamics, Phys. Rev. D 59, 084006 (1999), arXiv:gr-qc/9811091

    1999 arXiv

  132. [140]

    Buonanno and T

    A. Buonanno and T. Damour, Transition from inspiral to plunge in binary black hole coalescences, Phys. Rev. D 62, 064015 (2000), arXiv:gr-qc/0001013

    2000 arXiv

  133. [141]

    Cao and W.-B

    Z. Cao and W.-B. Han, Waveform model for an eccen- tric binary black hole based on the effective-one-body- numerical-relativity formalism, Phys. Rev. D96, 044028 (2017), arXiv:1708.00166 [gr-qc]

    2017 arXiv

  134. [142]

    X. Liu, Z. Cao, and Z.-H. Zhu, A higher-multipole gravitational waveform model for an eccentric binary black holes based on the effective-one-body-numerical- relativity formalism, Class. Quant. Grav. 39, 035009 (2022), arXiv:2102.08614 [gr-qc]

    2022 arXiv

  135. [143]

    Chiaramello and A

    D. Chiaramello and A. Nagar, Faithful analytical effective-one-body waveform model for spin-aligned, moderately eccentric, coalescing black hole binaries, Phys. Rev. D 101, 101501 (2020), arXiv:2001.11736 [gr- qc]

    2020 arXiv

  136. [144]

    Nagar, A

    A. Nagar, A. Bonino, and P. Rettegno, Effective one- body multipolar waveform model for spin-aligned, qua- sicircular, eccentric, hyperbolic black hole binaries, Phys. Rev. D 103, 104021 (2021), arXiv:2101.08624 [gr- qc]

    2021 arXiv

  137. [145]

    Khalil, A

    M. Khalil, A. Buonanno, J. Steinhoff, and J. Vines, Radiation-reaction force and multipolar waveforms for eccentric, spin-aligned binaries in the effective-one- body formalism, Phys. Rev. D 104, 024046 (2021), arXiv:2104.11705 [gr-qc]

    2021 arXiv

  138. [146]

    Ramos-Buades, A

    A. Ramos-Buades, A. Buonanno, M. Khalil, and S. Os- sokine, Effective-one-body multipolar waveforms for ec- centric binary black holes with nonprecessing spins, Phys. Rev. D 105, 044035 (2022), arXiv:2112.06952 [gr- qc]

    2022 arXiv

  139. [147]

    X. Liu, Z. Cao, and Z.-H. Zhu, Effective-one-body numerical-relativity waveform model for eccentric spin- precessing binary black hole coalescence, Class. Quant. Grav. 41, 195019 (2024), arXiv:2310.04552 [gr-qc]

    2024 arXiv

  140. [148]

    K. Paul, A. Maurya, Q. Henry, K. Sharma, P. Satheesh, Divyajyoti, P. Kumar, and C. K. Mishra, ESIGMAHM: An Eccentric, Spinning inspiral-merger-ringdown wave- form model with Higher Modes for the detection and characterization of binary black holes, (2024), arXiv:2409.13866 [gr-qc]

    2024 arXiv

  141. [149]

    W. E. East, S. T. McWilliams, J. Levin, and F. Pre- torius, Observing complete gravitational wave signals from dynamical capture binaries, Phys. Rev. D 87, 043004 (2013), arXiv:1212.0837 [gr-qc]

    2013 arXiv

  142. [150]

    E. A. Huerta et al., Complete waveform model for com- pact binaries on eccentric orbits, Phys. Rev. D 95, 024038 (2017), arXiv:1609.05933 [gr-qc]

    2017 arXiv

  143. [151]

    E. A. Huerta et al. , Eccentric, nonspinning, inspi- ral, Gaussian-process merger approximant for the de- tection and characterization of eccentric binary black hole mergers, Phys. Rev. D 97, 024031 (2018), arXiv:1711.06276 [gr-qc]

    2018 arXiv

  144. [152]

    Hinder, L

    I. Hinder, L. E. Kidder, and H. P. Pfeiffer, Eccentric bi- nary black hole inspiral-merger-ringdown gravitational waveform model from numerical relativity and post- Newtonian theory, Phys. Rev. D 98, 044015 (2018), arXiv:1709.02007 [gr-qc]

    2018 arXiv

  145. [153]

    Setyawati and F

    Y. Setyawati and F. Ohme, Adding eccentricity to quasi- circular binary-black-hole waveform models, Phys. Rev. D 103, 124011 (2021), arXiv:2101.11033 [gr-qc]

    2021 arXiv

  146. [154]

    Wang, Y.-C

    H. Wang, Y.-C. Zou, and Y. Liu, Phenomenological re- lationship between eccentric and quasicircular orbital binary black hole waveform, Phys. Rev. D 107, 124061 27 (2023), arXiv:2302.11227 [gr-qc]

    2023 arXiv

  147. [155]

    Lynch, M

    P. Lynch, M. van de Meent, and N. Warburton, Eccen- tric self-forced inspirals into a rotating black hole, Class. Quant. Grav. 39, 145004 (2022), arXiv:2112.05651 [gr- qc]

    2022 arXiv

  148. [156]

    M. L. Katz, A. J. K. Chua, L. Speri, N. Warbur- ton, and S. A. Hughes, Fast extreme-mass-ratio-inspiral waveforms: New tools for millihertz gravitational- wave data analysis, Phys. Rev. D 104, 064047 (2021), arXiv:2104.04582 [gr-qc]

    2021 arXiv

  149. [157]

    Cutler and E

    C. Cutler and E. E. Flanagan, Gravitational waves from merging compact binaries: How accurately can one extract the binary’s parameters from the inspiral wave form?, Phys. Rev. D 49, 2658 (1994), arXiv:gr- qc/9402014

    1994

  150. [158]

    LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration, LVK Algorithm Library - LALSuite, Free software (GPL) (2018)

    2018

  151. [159]

    Buonanno, B

    A. Buonanno, B. Iyer, E. Ochsner, Y. Pan, and B. S. Sathyaprakash, Comparison of post-Newtonian templates for compact binary inspiral signals in gravitational-wave detectors, Phys. Rev. D 80, 084043 (2009), arXiv:0907.0700 [gr-qc]

    2009 arXiv

  152. [160]

    K. G. Arun, A. Buonanno, G. Faye, and E. Ochsner, Higher-order spin effects in the amplitude and phase of gravitational waveforms emitted by inspiraling compact binaries: Ready-to-use gravitational waveforms, Phys. Rev. D 79, 104023 (2009), [Erratum: Phys.Rev.D 84, 049901 (201...

    2009 arXiv

  153. [161]

    Favata, C

    M. Favata, C. Kim, K. G. Arun, J. Kim, and H. W. Lee, Constraining the orbital eccentricity of inspiralling compact binary systems with Advanced LIGO, Phys. Rev. D 105, 023003 (2022), arXiv:2108.05861 [gr-qc]

    2022 arXiv

  154. [162]

    Damour and G

    T. Damour and G. Schaefer, Higher Order Relativistic Periastron Advances and Binary Pulsars, Nuovo Cim. B101, 127 (1988)

    1988

  155. [163]

    Sch¨ afer and N

    G. Sch¨ afer and N. Wex, Second post-Newtonian motion of compact binaries, Physics Letters A 174, 196 (1993)

    1993

  156. [164]

    Ramos-Buades, M

    A. Ramos-Buades, M. van de Meent, H. P. Pfeiffer, H. R. R¨ uter, M. A. Scheel, M. Boyle, and L. E. Kidder, Eccentric binary black holes: Comparing numerical rel- ativity and small mass-ratio perturbation theory, Phys. Rev. D 106, 124040 (2022), arXiv:2209.03390 [gr-qc]

    2022 arXiv

  157. [165]

    M. A. Shaikh, V. Varma, H. P. Pfeiffer, A. Ramos- Buades, and M. van de Meent, Defining eccentricity for gravitational wave astronomy, Phys. Rev. D 108, 104007 (2023), arXiv:2302.11257 [gr-qc]

    2023 arXiv

  158. [166]

    Mora and C

    T. Mora and C. M. Will, Numerically generated quasiequilibrium orbits of black holes: Circular or ec- centric?, Phys. Rev. D 66, 101501 (2002), arXiv:gr- qc/0208089

    2002

  159. [167]

    Mora and C

    T. Mora and C. M. Will, A PostNewtonian diagnos- tic of quasiequilibrium binary configurations of com- pact objects, Phys. Rev. D69, 104021 (2004), [Erratum: Phys.Rev.D 71, 129901 (2005)], arXiv:gr-qc/0312082

    2004 arXiv

  160. [168]

    Bonino, P

    A. Bonino, P. Schmidt, and G. Pratten, Mapping ec- centricity evolutions between numerical relativity and effective-one-body gravitational waveforms, Phys. Rev. D 110, 104002 (2024), arXiv:2404.18875 [gr-qc]

    2024 arXiv

  161. [169]

    Boschini, N

    M. Boschini, N. Loutrel, D. Gerosa, and G. Fumagalli, Orbital eccentricity in general relativity from catastro- phe theory, (2024), arXiv:2411.00098 [gr-qc]

    2024 arXiv

  162. [170]

    Ramos-Buades, S

    A. Ramos-Buades, S. Husa, G. Pratten, H. Estell´ es, C. Garc´ ıa-Quir´ os, M. Mateu-Lucena, M. Colleoni, and R. Jaume, First survey of spinning eccentric black hole mergers: Numerical relativity simulations, hybrid wave- forms, and parameter estimation, Phys. Rev. D 101, 08301...

    2020 arXiv

  163. [171]

    C. M. Will, Compact binary inspiral: Nature is perfectly happy with a circle, Class. Quant. Grav. 36, 195013 (2019), arXiv:1906.08064 [gr-qc]

    2019 arXiv

  164. [172]

    Memmesheimer, A

    R.-M. Memmesheimer, A. Gopakumar, and G. Schae- fer, Third post-Newtonian accurate generalized quasi- Keplerian parametrization for compact binaries in ec- centric orbits, Phys. Rev. D70, 104011 (2004), arXiv:gr- qc/0407049

    2004

  165. [173]

    Konigsdorffer and A

    C. Konigsdorffer and A. Gopakumar, Phasing of grav- itational waves from inspiralling eccentric binaries at the third-and-a-half post-Newtonian order, Phys. Rev. D 73, 124012 (2006), arXiv:gr-qc/0603056

    2006 arXiv

  166. [174]

    K. G. Arun, L. Blanchet, B. R. Iyer, and S. Sinha, Third post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact bi- naries in quasi-elliptical orbits, Phys. Rev. D80, 124018 (2009), arXiv:0908.3854 [gr-qc]

    2009 arXiv

  167. [175]

    Henry and M

    Q. Henry and M. Khalil, Spin effects in gravitational waveforms and fluxes for binaries on eccentric orbits to the third post-Newtonian order, Phys. Rev. D 108, 104016 (2023), arXiv:2308.13606 [gr-qc]

    2023 arXiv

  168. [176]

    Klein and P

    A. Klein and P. Jetzer, Spin effects in the phasing of gravitational waves from binaries on eccentric orbits, Phys. Rev. D 81, 124001 (2010), arXiv:1005.2046 [gr- qc]

    2010 arXiv

  169. [177]

    Sridhar, S

    O. Sridhar, S. Bhattacharyya, K. Paul, and C. K. Mishra, Spin effects in the phasing formula of eccentric compact binary inspirals till the third post-Newtonian order, (2024), arXiv:2412.10909 [gr-qc]

    2024 arXiv

  170. [178]

    Pai and K

    A. Pai and K. G. Arun, Singular value decomposition in parametrised tests of post-Newtonian theory, Class. Quant. Grav. 30, 025011 (2013), arXiv:1207.1943 [gr- qc]

    2013 arXiv

  171. [179]

    F. Ohme, A. B. Nielsen, D. Keppel, and A. Lundgren, Statistical and systematic errors for gravitational-wave inspiral signals: A principal component analysis, Phys. Rev. D 88, 042002 (2013), arXiv:1304.7017 [gr-qc]

    2013 arXiv

  172. [180]

    Tanaka and H

    T. Tanaka and H. Tagoshi, The Use of new coordinates for the template space in hierarchical search for gravi- tational waves from inspiraling binaries, Phys. Rev. D 62, 082001 (2000), arXiv:gr-qc/0001090

    2000 arXiv

  173. [181]

    B. J. Owen, Search templates for gravitational waves from inspiraling binaries: Choice of template spacing, Phys. Rev. D 53, 6749 (1996), arXiv:gr-qc/9511032

    1996 arXiv

  174. [182]

    Poisson and C

    E. Poisson and C. M. Will, Gravitational waves from in- spiraling compact binaries: Parameter estimation using second postNewtonian wave forms, Phys. Rev. D 52, 848 (1995), arXiv:gr-qc/9502040

    1995 arXiv

  175. [183]

    Keppel, A

    D. Keppel, A. P. Lundgren, B. J. Owen, and H. Zhu, Parameter space metric for 3.5 post-Newtonian gravitational-waves from compact binary inspirals, Phys. Rev. D 88, 063002 (2013), arXiv:1305.5381 [gr- qc]

    2013 arXiv

  176. [184]

    Kalaghatgi, P

    C. Kalaghatgi, P. Ajith, and K. G. Arun, Template- space metric for searches for gravitational waves from the inspiral, merger and ringdown of binary black holes, Phys. Rev. D 91, 124042 (2015), arXiv:1501.04418 [gr- qc]

    2015 arXiv

  177. [185]

    Harry and A

    I. Harry and A. Lundgren, Failure of the Fisher ma- trix when including tidal terms: Considering con- 28 struction of template banks of tidally deformed bi- nary neutron stars, Phys. Rev. D 104, 043008 (2021), arXiv:2101.01091 [gr-qc]

    2021 arXiv

  178. [186]

    org/LIGO-T2000012/public

    Noise curves used for Simulations, https://dcc.ligo. org/LIGO-T2000012/public

  179. [187]

    Cannon, A

    K. Cannon, A. Chapman, C. Hanna, D. Keppel, A. C. Searle, and A. J. Weinstein, Singular value decomposition applied to compact binary coalescence gravitational-wave signals, Phys. Rev. D 82, 044025 (2010), arXiv:1005.0012 [gr-qc]

    2010 arXiv

  180. [188]

    S. E. Field, C. R. Galley, F. Herrmann, J. S. Hes- thaven, E. Ochsner, and M. Tiglio, Reduced basis cata- logs for gravitational wave templates, Phys. Rev. Lett. 106, 221102 (2011), arXiv:1101.3765 [gr-qc]

    2011 arXiv

  181. [189]

    Kulkarni, K

    S. Kulkarni, K. S. Phukon, A. Reza, S. Bose, A. Das- gupta, D. Krishnaswamy, and A. S. Sengupta, Ran- dom projections in gravitational wave searches of compact binaries, Phys. Rev. D 99, 101503 (2019), arXiv:1801.04506 [gr-qc]

    2019 arXiv

  182. [190]

    J. H. Conway and N. J. A. Sloane, Sphere Packings, Lattices and Groups (Springer New York, NY, 1993)

    1993

  183. [191]

    Wette, Lattice template placement for coherent all- sky searches for gravitational-wave pulsars, Phys

    K. Wette, Lattice template placement for coherent all- sky searches for gravitational-wave pulsars, Phys. Rev. D 90, 122010 (2014), arXiv:1410.6882 [gr-qc]

    2014 arXiv

  184. [192]

    Virtanen et al

    P. Virtanen et al. , SciPy 1.0–Fundamental Algorithms for Scientific Computing in Python, Nature Meth. 17, 261 (2020), arXiv:1907.10121 [cs.MS]

    2020 arXiv

  185. [193]

    Ajith et al

    P. Ajith et al. , Inspiral-merger-ringdown waveforms for black-hole binaries with non-precessing spins, Phys. Rev. Lett. 106, 241101 (2011), arXiv:0909.2867 [gr-qc]

    2011 arXiv

  186. [194]

    Damour, B

    T. Damour, B. R. Iyer, and B. S. Sathyaprakash, Improved filters for gravitational waves from inspi- ralling compact binaries, Phys. Rev. D 57, 885 (1998), arXiv:gr-qc/9708034

    1998 arXiv

  187. [195]

    T. A. Apostolatos, Search templates for gravitational waves from precessing, inspiraling binaries, Phys. Rev. D 52, 605 (1995)

    1995

  188. [196]

    A. Nitz, I. Harry, D. Brown, C. M. Biwer, J. Willis, T. D. Canton, C. Capano, T. Dent, L. Pekowsky, G. S. C. Davies, S. De, M. Cabero, S. Wu, A. R. Williamson, B. Machenschalk, D. Macleod, F. Pan- narale, P. Kumar, S. Reyes, D. Finstad, S. Kumar, M. T´ apai, L. Singer, P. Kuma...

    2024

  189. [197]

    A. H. Nitz, A. Lundgren, D. A. Brown, E. Ochsner, D. Keppel, and I. W. Harry, Accuracy of gravitational waveform models for observing neutron-star–black-hole binaries in Advanced LIGO, Phys. Rev. D 88, 124039 (2013), arXiv:1307.1757 [gr-qc]

    2013 arXiv

  190. [198]

    Buonanno, Y.-b

    A. Buonanno, Y.-b. Chen, and M. Vallisneri, Detect- ing gravitational waves from precessing binaries of spin- ning compact objects: Adiabatic limit, Phys. Rev. D 67, 104025 (2003), [Erratum: Phys.Rev.D 74, 029904 (2006)], arXiv:gr-qc/0211087

    2003 arXiv

  191. [199]

    Fumagalli, I

    G. Fumagalli, I. Romero-Shaw, D. Gerosa, V. De Ren- zis, K. Kritos, and A. Olejak, Residual eccentricity as a systematic uncertainty on the formation channels of binary black holes, Phys. Rev. D 110, 063012 (2024), arXiv:2405.14945 [astro-ph.HE]

    2024 arXiv

  192. [200]

    Abbott et al

    R. Abbott et al. (LIGO Scientific, Virgo), GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses, Phys. Rev. D 102, 043015 (2020), arXiv:2004.08342 [astro-ph.HE]

    2020 arXiv

  193. [201]

    Hannam et al

    M. Hannam et al. , General-relativistic precession in a black-hole binary, Nature 610, 652 (2022), arXiv:2112.11300 [gr-qc]

    2022 arXiv

  194. [202]

    B. P. Abbott et al. (LIGO Scientific, Virgo), GW170817: Observation of Gravitational Waves from a Binary Neu- tron Star Inspiral, Phys. Rev. Lett. 119, 161101 (2017), arXiv:1710.05832 [gr-qc]

    2017 arXiv

  195. [203]

    Capano, Y

    C. Capano, Y. Pan, and A. Buonanno, Impact of higher harmonics in searching for gravitational waves from nonspinning binary black holes, Phys. Rev. D 89, 102003 (2014), arXiv:1311.1286 [gr-qc]

    2014 arXiv

  196. [204]

    Moreno-Garrido, E

    C. Moreno-Garrido, E. Mediavilla, and J. Buitrago, Gravitational radiation from point masses in elliptical orbits: spectral analysis and orbital parameters, Mon. Not. Roy. Soc. 274, 115 (1995)

    1995

  197. [205]

    Moore, T

    B. Moore, T. Robson, N. Loutrel, and N. Yunes, To- wards a Fourier domain waveform for non-spinning bi- naries with arbitrary eccentricity, Class. Quant. Grav. 35, 235006 (2018), arXiv:1807.07163 [gr-qc]

    2018 arXiv

  198. [206]

    McInnes, J

    L. McInnes, J. Healy, and J. Melville, UMAP: Uni- form Manifold Approximation and Projection for Dimension Reduction, , arXiv:1802.03426 (2018), arXiv:1802.03426 [stat.ML]

    2018 arXiv

  199. [207]

    D. E. Rumelhart and J. L. McClelland, Learning in- ternal representations by error propagation, in Parallel Distributed Processing: Explorations in the Microstruc- ture of Cognition: Foundations (1987) pp. 318–362

    1987

  200. [208]

    A. H. Nitz, Robust, Rapid, and Simple Gravitational- wave Parameter Estimation, (2024), arXiv:2410.05190 [astro-ph.IM]

    2024 arXiv

  201. [209]

    C. K. Mishra, A. Kela, K. G. Arun, and G. Faye, Ready- to-use post-Newtonian gravitational waveforms for bi- nary black holes with nonprecessing spins: An update, Phys. Rev. D 93, 084054 (2016), arXiv:1601.05588 [gr- qc]

    2016 arXiv

  202. [210]

    Damour, B

    T. Damour, B. R. Iyer, and B. S. Sathyaprakash, A Comparison of search templates for gravitational waves from binary inspiral, Phys. Rev. D 63, 044023 (2001), [Erratum: Phys.Rev.D 72, 029902 (2005)], arXiv:gr- qc/0010009

    2001

  203. [211]

    Damour, B

    T. Damour, B. R. Iyer, and B. S. Sathyaprakash, A Comparison of search templates for gravitational waves from binary inspiral - 3.5PN update, Phys. Rev. D 66, 027502 (2002), arXiv:gr-qc/0207021

    2002 arXiv

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