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arxiv: 2512.10803 · v2 · submitted 2025-12-11 · 🌀 gr-qc

Detection of GW200105 with a targeted eccentric search

Khun Sang Phukon , Patricia Schmidt , Gonzalo Morras , Geraint Pratten This is my paper

Pith reviewed 2026-05-16 23:03 UTC · model grok-4.3

classification 🌀 gr-qc
keywords gravitational wavesGW200105eccentric binaryneutron star black holematched filter searchdynamical formationorbital eccentricity
0
0 comments X p. Extension

The pith

A targeted eccentric search recovers GW200105 at SNR 13.4 with false alarm rate below one per thousand years.

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

The paper demonstrates that matched-filter searches using non-eccentric templates can miss or downgrade the significance of events that carry orbital eccentricity. By applying a targeted search with eccentric waveforms to the same data, the authors recover GW200105 as the loudest trigger. The recovered parameters line up with earlier Bayesian results, reinforcing that the binary formed through dynamical channels rather than isolated evolution.

Core claim

The eccentric search identifies GW200105 as the most significant event with a signal-to-noise ratio of 13.4 and a false alarm rate of less than 1 in 1000 years. The best-matching template parameters are consistent with the Bayesian inference result, supporting the interpretation of GW200105 as an NSBH that formed through dynamical mechanisms including hierarchical triples and not via isolated binary evolution.

What carries the argument

Targeted eccentric template bank and search pipeline that matches waveforms containing orbital eccentricity at 20 Hz to the gravitational-wave data.

If this is right

  • The event significance rises when eccentricity is included in the templates.
  • Best-fit eccentric parameters agree with independent Bayesian estimates of the same event.
  • The result favors dynamical formation channels over isolated binary evolution for this NSBH system.
  • Standard circular searches can under-report the detectability of eccentric mergers.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar targeted eccentric searches could be run on other marginal candidates to test whether eccentricity was overlooked.
  • Routine inclusion of eccentric templates in broad searches may be needed to maintain sensitivity to dynamically formed binaries.
  • The consistency between the search template and Bayesian posterior suggests that future parameter estimation can be initialized directly from search results when eccentricity is present.

Load-bearing premise

The eccentric template bank and pipeline are correctly calibrated so that they do not artificially inflate the significance of a previously identified candidate.

What would settle it

Injection of known eccentric signals into real detector noise followed by recovery with both eccentric and non-eccentric pipelines, checking whether the eccentric pipeline systematically returns higher significance than expected from the injections.

Figures

Figures reproduced from arXiv: 2512.10803 by Geraint Pratten, Gonzalo Morras, Khun Sang Phukon, Patricia Schmidt.

Figure 1
Figure 1. Figure 1: FIG. 1. Density distribution of the templates in the eccentric template bank for the targeted search, shown in the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. The SNR, [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. The ( [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. The ratio of the sensitive spacetime volume be [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Reweighted SNRs ˆρ [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
read the original abstract

The neutron star -- black hole (NSBH) binary GW200105 was recently found to have significant residual orbital eccentricity at a gravitational-wave frequency of 20 Hz~\cite{Morras:2025xfu}. The event was originally identified with moderate significance by matched-filter searches that employ non-eccentric templates. The neglect of relevant physical effects, such as orbital eccentricity, can severely reduce the sensitivity of the search and, consequently, also the significance of an event candidate. Here, we present a targeted eccentric search for GW200105. The eccentric search identifies GW200105 as the most significant event with a signal-to-noise ratio of $13.4$ and a false alarm rate of less than 1 in 1000 years. The best-matching template parameters are consistent with the Bayesian inference result, supporting the interpretation of GW200105 as an NSBH that formed through dynamical mechanisms including hierarchical triples and not via isolated binary evolution.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript presents a targeted eccentric matched-filter search for the known NSBH candidate GW200105. Using an eccentric template bank, the search recovers the event as the most significant trigger with SNR 13.4 and FAR < 1/1000 yr. The best-fit parameters are reported as consistent with prior Bayesian results, supporting a dynamical formation channel involving eccentricity at 20 Hz rather than isolated binary evolution.

Significance. If the eccentric template bank construction, ranking statistic, and background estimation (via time-slides or Monte Carlo) are robust, the result demonstrates that neglecting eccentricity can reduce search sensitivity and provides independent support for residual eccentricity in GW200105. This strengthens evidence for dynamical formation mechanisms in NSBH systems and highlights the utility of targeted eccentric searches for known candidates. The explicit methods for bank construction and background estimation aid reproducibility.

major comments (2)
  1. [Targeted search and background estimation] Targeted search section: the reported FAR < 1/1000 yr for a search centered on a previously identified candidate requires explicit validation that the background distribution accounts for the reduced search volume; without injection studies or a direct comparison to the all-sky non-eccentric FAR, the significance gain could be partly due to targeting rather than improved waveform fidelity.
  2. [Results and parameter comparison] Parameter recovery: the claim that best-matching template parameters are consistent with Bayesian inference (Morras:2025xfu) is central to the formation-channel interpretation, yet no quantitative table or overlap metric (e.g., 90% credible interval overlap for eccentricity) is referenced; this leaves the consistency statement qualitative.
minor comments (2)
  1. [Introduction] The abstract states the 20 Hz reference frequency for eccentricity; repeat this definition at first mention in the main text for clarity.
  2. [Methods] Ensure SNR and FAR are defined at first use and that the ranking statistic formula is given explicitly (e.g., as Eq. (X)) rather than only described.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive review and recommendation for minor revision. We address each major comment below and will revise the manuscript to incorporate the suggested clarifications and additions.

read point-by-point responses

  1. Referee: [Targeted search and background estimation] Targeted search section: the reported FAR < 1/1000 yr for a search centered on a previously identified candidate requires explicit validation that the background distribution accounts for the reduced search volume; without injection studies or a direct comparison to the all-sky non-eccentric FAR, the significance gain could be partly due to targeting rather than improved waveform fidelity.

    Authors: We agree that explicit validation of the background estimation for the targeted search is necessary to distinguish the contribution of the eccentric templates from the effect of the reduced search volume. In the revised manuscript, we will expand the Targeted search section to detail how the background is computed via time-slides restricted to the targeted parameter space and sky location. We will also add results from a set of injection studies performed within the same targeted volume to confirm the reported FAR, and include a direct numerical comparison of the targeted eccentric FAR to the all-sky non-eccentric FAR reported in the original discovery papers. revision: yes

  2. Referee: [Results and parameter comparison] Parameter recovery: the claim that best-matching template parameters are consistent with Bayesian inference (Morras:2025xfu) is central to the formation-channel interpretation, yet no quantitative table or overlap metric (e.g., 90% credible interval overlap for eccentricity) is referenced; this leaves the consistency statement qualitative.

    Authors: We accept that the consistency statement would be strengthened by quantitative metrics. In the revised manuscript, we will add a new table (or subsection) that lists the best-fit parameters from the eccentric matched-filter search together with the corresponding 90% credible intervals from the Bayesian analysis of Morras:2025xfu. The table will include overlap fractions or compatibility metrics for eccentricity, component masses, and spins, allowing readers to assess the agreement quantitatively. revision: yes

Circularity Check

0 steps flagged

Targeted eccentric search supplies independent significance via explicit pipeline

full rationale

The paper's central claim is the output of a targeted search pipeline (bank construction, ranking statistic, background estimation via time-slides or Monte-Carlo) applied to the strain data. The reported SNR 13.4 and FAR < 1/1000 yr are direct results of that pipeline, not re-derivations of prior Bayesian posteriors. Consistency with the cited Morras:2025xfu parameters is presented only as a post-hoc check, not as an input that forces the detection statistic. No self-definitional loop, fitted-parameter renaming, or load-bearing self-citation chain appears in the derivation of the significance; the methods section supplies the independent calibration steps required by the skeptic analysis.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The claim rests on the accuracy of eccentric waveform models for NSBH systems and on the statistical calibration of the targeted search pipeline; no free parameters or invented entities are explicitly introduced in the abstract.

axioms (1)
  • domain assumption General relativity provides accurate waveform models for eccentric NSBH binaries at the relevant frequencies
    Invoked by the use of eccentric templates to claim detection.

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Reference graph

Works this paper leans on

70 extracted references · 70 canonical work pages · cited by 5 Pith papers · 30 internal anchors

  1. [1]

    Morras, G

    G. Morras, G. Pratten, and P. Schmidt, Orbital eccentric- ity in a neutron star - black hole binary, arXiv:2503.15393 [astro-ph.HE] (2025)

    work page arXiv 2025

  2. [2]

    Advanced LIGO

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

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  3. [3]

    Advanced Virgo: a 2nd generation interferometric gravitational wave detector

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

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  4. [4]

    Akutsuet al., Progress of Theoretical and Experi- mental Physics2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]

    T. Akutsuet al.(KAGRA), Overview of KAGRA: Detec- tor design and construction history, PTEP2021, 05A101 10 (2021), arXiv:2005.05574 [physics.ins-det]

    work page arXiv 2021

  5. [5]

    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. D88, 043007 (2013), arXiv:1306.6747 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  6. [6]

    Somiya (KAGRA), Detector configuration of KA- GRA: The Japanese cryogenic gravitational-wave de- tector, Class

    K. Somiya (KAGRA), Detector configuration of KA- GRA: The Japanese cryogenic gravitational-wave de- tector, Class. Quant. Grav.29, 124007 (2012), arXiv:1111.7185 [gr-qc]

    work page arXiv 2012

  7. [7]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Updating the Gravitational-Wave Tran- sient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, arXiv:2508.18082 [gr-qc] (2025)

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  8. [8]

    GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run

    R. Abbottet al.(KAGRA, VIRGO, LIGO Scien- tific), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run, Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  9. [9]

    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 Compact Binary Mergers, Astrophys. J.946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]

    work page arXiv 2023

  10. [10]

    Olsen, T

    S. Olsen, T. Venumadhav, J. Mushkin, J. Roulet, B. Za- ckay, and M. Zaldarriaga, New binary black hole mergers in the LIGO-Virgo O3a data, Phys. Rev. D106, 043009 (2022), arXiv:2201.02252 [astro-ph.HE]

    work page arXiv 2022

  11. [11]

    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, Phys. Rev. D111, 024049 (2025), arXiv:2311.06061 [gr-qc]

    work page arXiv 2025

  12. [12]

    Capoteet al., Advanced LIGO detector performance in the fourth observing run, Phys

    E. Capoteet al., Advanced LIGO detector performance in the fourth observing run, Phys. Rev. D111, 062002 (2025), arXiv:2411.14607 [gr-qc]

    work page arXiv 2025

  13. [13]

    (LIGO Instrument Science Collaboration) 2025 Class

    S. Soniet al.(LIGO), LIGO Detector Characterization in the first half of the fourth Observing run, Class. Quant. Grav.42, 085016 (2025), arXiv:2409.02831 [astro-ph.IM]

    work page arXiv 2025

  14. [14]

    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

    work page arXiv 2012

  15. [15]

    Toward Early-Warning Detection of Gravitational Waves from Compact Binary Coalescence

    K. Cannonet al., Toward Early-Warning Detection of Gravitational Waves from Compact Binary Coalescence, Astrophys. J.748, 136 (2012), arXiv:1107.2665 [astro- ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  16. [16]

    Low-latency analysis pipeline for compact binary coalescences in the advanced gravitational wave detector era

    T. Adams, D. Buskulic, V. Germain, G. M. Guidi, F. Marion, M. Montani, B. Mours, F. Piergiovanni, and 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:1512.02864 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  17. [17]

    J. Luan, S. Hooper, L. Wen, and Y. Chen, Towards low- latency real-time detection of gravitational waves from compact binary coalescences in the era of advanced de- tectors, Phys. Rev. D85, 102002 (2012), arXiv:1108.3174 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  18. [18]

    Lense and H

    J. Lense and H. Thirring, Ueber den Einfluss der Eigenro- tation der Zentralkoerper auf die Bewegung der Planeten und Monde nach der Einsteinschen Gravitationstheorie, Phys. Z.19, 156 (1918)

    work page 1918

  19. [19]

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

    work page 1963

  20. [20]

    A. H. Nitz, A. Lenon, and D. A. Brown, Search for Eccen- tric 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]

    work page arXiv 2019

  21. [21]

    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]

    work page arXiv 2021

  22. [22]

    A. H. Nitz and Y.-F. Wang, Search for gravitational waves from the coalescence of sub-solar mass and ec- centric compact binaries, Astrophys. J.915, 54 (2021), arXiv:2102.00868 [astro-ph.HE]

    work page arXiv 2021

  23. [23]

    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, Phys. Rev. D111, 103018 (2025), arXiv:2311.00242 [astro-ph.HE]

    work page arXiv 2025

  24. [24]

    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. D108, 123016 (2023), arXiv:2303.17364 [gr-qc]

    work page arXiv 2023

  25. [25]

    Schmidtet al., Searching for gravitational-wave signals from precessing black hole binaries with the GstLAL pipeline, Phys

    S. Schmidtet al., Searching for gravitational-wave signals from precessing black hole binaries with the GstLAL pipeline, Phys. Rev. D110, 023038 (2024), arXiv:2403.17186 [gr-qc]

    work page arXiv 2024

  26. [26]

    Pal and K

    S. Pal and K. R. Nayak, Swarm-intelligent search for gravitational waves from eccentric binary mergers, Phys. Rev. D110, 042003 (2024), arXiv:2307.03736 [gr-qc]

    work page arXiv 2024

  27. [27]

    K. S. Phukon, P. Schmidt, and G. Pratten, Geomet- ric template bank for the detection of spinning low- mass compact binaries with moderate orbital eccentric- ity, Phys. Rev. D111, 043040 (2025), arXiv:2412.06433 [gr-qc]

    work page arXiv 2025

  28. [28]

    Wang and A

    Y.-F. Wang and A. H. Nitz, Search for Gravitational Waves from Eccentric Binary Black Holes with an Effective-one-body Template, Astrophys. J.993, 215 (2025), arXiv:2508.05018 [gr-qc]

    work page arXiv 2025

  29. [29]

    B. P. Abbottet 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]

    work page arXiv 2019

  30. [30]

    A. G. Abacet 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]

    work page arXiv 2024

  31. [31]

    Spin-Orbit Misalignment in Close Binaries with Two Compact Objects

    V. Kalogera, Spin orbit misalignment in close binaries with two compact objects, Astrophys. J.541, 319 (2000), arXiv:astro-ph/9911417

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  32. [32]

    The Formation of Eccentric Compact Binary Inspirals and the Role of Gravitational Wave Emission in Binary-Single Stellar Encounters

    J. Samsing, M. MacLeod, and E. Ramirez-Ruiz, The Formation of Eccentric Compact Binary Inspirals and the Role of Gravitational Wave Emission in Binary- Single Stellar Encounters, Astrophys. J.784, 71 (2014), arXiv:1308.2964 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  33. [33]

    C. L. Rodriguez, M. Zevin, C. Pankow, V. Kalogera, and F. A. Rasio, Illuminating Black Hole Binary Formation Channels with Spins in Advanced LIGO, Astrophys. J. Lett.832, L2 (2016), arXiv:1609.05916 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  34. [34]

    Orbital eccentricities in primordial black holes binaries

    I. Cholis, E. D. Kovetz, Y. Ali-Ha¨ ımoud, S. Bird, M. Kamionkowski, J. B. Mu˜ noz, and A. Raccanelli, Orbital eccentricities in primordial black hole binaries, 11 Phys. Rev. D94, 084013 (2016), arXiv:1606.07437 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  35. [35]

    Stegmann and J

    J. Stegmann and J. Klencki, Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neu- tron Star–Black Hole Mergers Form through Triple Star Evolution, Astrophys. J. Lett.991, L54 (2025), arXiv:2506.09121 [astro-ph.HE]

    work page arXiv 2025

  36. [36]

    The population of merging compact binaries inferred using gravitational waves through GWTC-3

    R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3, Phys. Rev. X13, 011048 (2023), arXiv:2111.03634 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  37. [37]

    M. d. L. Planas, S. Husa, A. Ramos-Buades, and J. Va- lencia, First eccentric inspiral-merger-ringdown analy- sis of neutron star-black hole mergers, arXiv:2506.01760 [astro-ph.HE] (2025)

    work page arXiv 2025

  38. [38]

    Jan, B.-J

    A. Jan, B.-J. Tsao, R. O’Shaughnessy, D. Shoe- maker, and P. Laguna, GW200105: A detailed study of eccentricity in the neutron star-black hole binary, arXiv:2508.12460 [gr-qc] (2025)

    work page arXiv 2025

  39. [39]

    Kacanja, K

    K. Kacanja, K. Soni, and A. H. Nitz, Eccentricity signa- tures in LIGO-Virgo-KAGRA’s BNS and NSBH binaries, arXiv:2508.00179 [gr-qc] (2025)

    work page arXiv 2025

  40. [40]

    Abbottet al.(LIGO Scientific, KAGRA, VIRGO), As- trophys

    R. Abbottet al.(LIGO Scientific, KAGRA, VIRGO), Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences, Astrophys. J. Lett.915, L5 (2021), arXiv:2106.15163 [astro-ph.HE]

    work page arXiv 2021

  41. [41]

    Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Astrophys

    R. Abbottet 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]

    work page arXiv 2023

  42. [42]

    (LIGO Instrument Science Collaboration) 2021 Class

    D. Daviset al.(LIGO), LIGO detector characterization in the second and third observing runs, Class. Quant. Grav.38, 135014 (2021), arXiv:2101.11673 [astro-ph.IM]

    work page arXiv 2021

  43. [43]

    Acerneseet al.(Virgo), Virgo Detector Characteriza- tion and Data Quality during the O3 run, Class

    F. Acerneseet al.(Virgo), Virgo Detector Characteriza- tion and Data Quality during the O3 run, Class. Quant. Grav.40, 185006 (2023), arXiv:2205.01555 [gr-qc]

    work page arXiv 2023

  44. [44]

    Validating gravitational-wave detections: The Advanced LIGO hardware injection system

    C. Biweret al., Validating gravitational-wave detec- tions: The Advanced LIGO hardware injection system, Phys. Rev. D95, 062002 (2017), arXiv:1612.07864 [astro- ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  45. [45]

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

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  46. [46]

    A. H. Nitz, T. Dent, T. Dal Canton, S. Fairhurst, and D. A. Brown, Detecting binary compact-object mergers with gravitational waves: Understanding and Improving the sensitivity of the PyCBC search, Astrophys. J.849, 118 (2017), arXiv:1705.01513 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  47. [47]

    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. D102, 022004 (2020), arXiv:2002.08291 [astro-ph.HE]

    work page arXiv 2020

  48. [48]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Methods for Identifying and Characterizing Gravitational-wave Transients, arXiv:2508.18081 [gr-qc] (2025)

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  49. [49]

    Gravitational-wave phasing for low-eccentricity inspiralling compact binaries to 3PN order

    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. D93, 124061 (2016), arXiv:1605.00304 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  50. [50]

    Morras, G

    G. Morras, G. Pratten, and P. Schmidt, Improved post- Newtonian waveform model for inspiralling precessing- eccentric compact binaries, Phys. Rev. D111, 084052 (2025), arXiv:2502.03929 [gr-qc]

    work page arXiv 2025

  51. [51]

    Inspiral-merger-ringdown waveforms for black-hole binaries with non-precessing spins

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

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  52. [52]

    Favata, C

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

    work page arXiv 2022

  53. [53]

    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. D79, 104023 (2009), [Erratum: Phys.Rev.D 84, 049901 (2011)], arXiv:0810.5336 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  54. [54]

    Comparison of post-Newtonian templates for compact binary inspiral signals in gravitational-wave detectors

    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. D80, 084043 (2009), arXiv:0907.0700 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  55. [55]

    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. D86, 084017 (2012), arXiv:1207.6406 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  56. [56]

    I. W. Harry, A. H. Nitz, D. A. Brown, A. P. Lund- gren, E. Ochsner, and D. Keppel, Investigating the effect of precession on searches for neutron-star-black-hole bi- naries with Advanced LIGO, Phys. Rev. D89, 024010 (2014), arXiv:1307.3562 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  57. [57]

    Searching for gravitational waves from binary coalescence

    S. Babaket al., Searching for gravitational waves from binary coalescence, Phys. Rev. D87, 024033 (2013), arXiv:1208.3491 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  58. [58]

    A chi-squared time-frequency discriminator for gravitational wave detection

    B. Allen,χ 2 time-frequency discriminator for gravita- tional wave detection, Phys. Rev. D71, 062001 (2005), arXiv:gr-qc/0405045

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  59. [59]

    Mozzon, L

    S. Mozzon, L. K. Nuttall, A. Lundgren, T. Dent, S. Kumar, and A. H. Nitz, Dynamic normalization for compact binary coalescence searches in non-stationary noise, Classical and Quantum Gravity37, 215014 (2020), arXiv:2002.09407 [astro-ph.IM]

    work page arXiv 2020

  60. [60]

    A. H. Nitz, T. Dent, G. S. Davies, S. Kumar, C. D. Capano, I. Harry, S. Mozzon, L. Nuttall, A. Lundgren, and M. T´ apai, 2-OGC: Open Gravitational-wave Cata- log of binary mergers from analysis of public Advanced LIGO and Virgo data, Astrophys. J.891, 123 (2020), arXiv:1910.05331 [astro-ph.HE]

    work page arXiv 2020

  61. [61]

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

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  62. [62]

    Likelihood-ratio ranking of gravitational-wave candidates in a non-Gaussian background

    R. Biswaset al., Likelihood-ratio ranking of gravitational-wave candidates in a non-Gaussian back- ground, Phys. Rev. D85, 122008 (2012), arXiv:1201.2959 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  63. [63]

    G. S. C. Davies and I. W. Harry, Establishing significance of gravitational-wave signals from a single observatory in the PyCBC offline search, Class. Quant. Grav.39, 215012 (2022), arXiv:2203.08545 [gr-qc]

    work page arXiv 2022

  64. [64]

    Optimizing gravitational-wave searches for a population of coalescing binaries: Intrinsic parameters

    T. Dent and J. Veitch, Optimizing gravitational-wave searches for a population of coalescing binaries: In- trinsic parameters, Phys. Rev. D89, 062002 (2014), arXiv:1311.7174 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  65. [65]

    Kumar and T

    P. Kumar and T. Dent, Optimized search for a binary black hole merger population in LIGO-Virgo O3 data, 12 Phys. Rev. D110, 043036 (2024), arXiv:2403.10439 [gr- qc]

    work page arXiv 2024

  66. [66]

    Essick, P

    R. Essick, P. Godwin, C. Hanna, L. Blackburn, and E. Katsavounidis, iDQ: Statistical Inference of Non- Gaussian Noise with Auxiliary Degrees of Freedom in Gravitational-Wave Detectors, Mach. Learn.: Sci. Tech- nol.2, 015004 (2020), arXiv:2005.12761 [astro-ph.IM]

    work page arXiv 2020

  67. [67]

    Estimation of the Sensitive Volume for Gravitational-wave Source Populations Using Weighted Monte Carlo Integration

    V. Tiwari, Estimation of the Sensitive Volume for Gravitational-wave Source Populations Using Weighted Monte Carlo Integration, Class. Quant. Grav.35, 145009 (2018), arXiv:1712.00482 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  68. [68]

    B. P. Abbottet al.(LIGO Scientific, Virgo), GW150914: First results from the search for binary black hole coa- lescence with Advanced LIGO, Phys. Rev. D93, 122003 (2016), arXiv:1602.03839 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  69. [69]

    R. Essicket al., Compact Binary Coalescence Sensitivity Estimates with Injection Campaigns during the LIGO- Virgo-KAGRA Collaborations’ Fourth Observing Run, arXiv:2508.10638 [gr-qc] (2025)

    work page arXiv 2025

  70. [70]

    Zevin, I

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

    work page arXiv 2021