Recognition: 2 theorem links
· Lean TheoremGWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs
Pith reviewed 2026-05-12 14:03 UTC · model grok-4.3
The pith
LIGO and Virgo detected gravitational waves from ten compact binary mergers across their first two observing runs and derived initial merger rate estimates.
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
During the first observing run, gravitational waves from three binary black hole mergers were detected. The second observing run saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to seven binary black hole mergers, four of which are reported here for the first time. For all significant events, estimates of the source properties are provided, with total masses ranging from 18.6 to 84.4 solar masses and distances from 320 to 2840 Mpc. From these results, merger rates at the 90 percent confidence level are inferred as 110 to 3840 Gpc^{-3} y^{-1} for binary neutron stars and 9.7 to 101 Gpc^{-3} y^{-1} for binary black holes, along with a 610 Gpc^{-3}
What carries the argument
Three gravitational-wave searches for coalescing compact binaries with component masses above one solar mass, combined with parameter estimation for source properties and rate inference from the observed events and search sensitivity.
If this is right
- The ten events establish a detection rate of roughly one significant merger per 15 days of searched data.
- Binary black hole total masses span 18.6 to 84.4 solar masses at distances up to several thousand Mpc.
- A 90 percent upper limit of 610 Gpc^{-3} y^{-1} is placed on neutron star-black hole merger rates.
- Marginal candidates with false alarm rates below one per 30 days are listed for further study.
Where Pith is reading between the lines
- These early rates provide a baseline that future runs can use to test whether merger rates evolve with redshift.
- The first binary neutron star event supplies a concrete anchor for models linking gravitational-wave signals to electromagnetic counterparts.
- The absence of neutron star-black hole detections already constrains the relative abundance of such mixed systems.
Load-bearing premise
Merger rate estimates depend on assuming fixed population distributions for the sources and accurate modeling of search sensitivity and detector noise without major unaccounted biases.
What would settle it
Observing a number of events in a later run that falls well outside the range predicted by these rates, after accounting for improved detector sensitivity, would indicate the current rate intervals are incorrect.
read the original abstract
We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1$\mathrm{M}_\odot$ during the first and second observing runs of the Advanced gravitational-wave detector network. During the first observing run (O1), from September $12^\mathrm{th}$, 2015 to January $19^\mathrm{th}$, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November $30^\mathrm{th}$, 2016 to August $25^\mathrm{th}$, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818 and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between $18.6_{-0.7}^{+3.2}\mathrm{M}_\odot$, and $84.4_{-11.1}^{+15.8} \mathrm{M}_\odot$, and range in distance between $320_{-110}^{+120}$ Mpc and $2840_{-1360}^{+1400}$ Mpc. No neutron star - black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of $110\, -\, 3840$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$ for binary neutron stars and $9.7\, -\, 101$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$ for binary black holes assuming fixed population distributions, and determine a neutron star - black hole merger rate 90% upper limit of $610$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The manuscript presents the GWTC-1 catalog compiling results from three independent gravitational-wave searches for compact binary coalescences (component masses >1 M_⊙) in LIGO/Virgo data from O1 (Sep 2015–Jan 2016) and O2 (Nov 2016–Aug 2017). It reports three binary black hole (BBH) detections in O1, seven BBH detections (four new) plus the first binary neutron star (BNS) detection in O2, provides Bayesian parameter estimates for all events (total BBH masses 18.6–84.4 M_⊙, distances 320–2840 Mpc), lists marginal candidates (FAR <1/30 days), and infers 90% credible intervals on merger rates of 110–3840 Gpc^{-3} y^{-1} (BNS) and 9.7–101 Gpc^{-3} y^{-1} (BBH) under fixed population distributions, plus a 610 Gpc^{-3} y^{-1} upper limit for neutron star–black hole mergers.
Significance. If the reported detections and conditional rates hold, the work is significant as the first public catalog of gravitational-wave transients from compact binaries. It transitions the field from individual event papers to population-level results, includes the landmark GW170817 BNS event, and supplies source parameters and rates that have anchored subsequent astrophysical and fundamental-physics studies. The use of three search pipelines and standard Bayesian parameter estimation on real strain data provides internal cross-checks; the explicit conditioning of rates on fixed population models is clearly stated.
minor comments (3)
- [Abstract] Abstract: the summary statistic 'approximately one gravitational-wave detection per 15 days of data searched' aggregates O1 and O2; a per-run breakdown would allow readers to evaluate detection-rate evolution without consulting the full text.
- [Abstract] Abstract: the BBH total-mass and distance ranges (18.6–84.4 M_⊙ and 320–2840 Mpc) are given without event labels; cross-referencing the extremes to specific events (e.g., GW170729) in the abstract would improve immediate readability.
- [Abstract] Abstract: the BNS rate interval (110–3840 Gpc^{-3} y^{-1}) is driven by a single event; a brief parenthetical note on the dominant uncertainty source would clarify the breadth of the interval for non-specialist readers.
Simulated Author's Rebuttal
We thank the referee for their positive summary of the GWTC-1 manuscript, recognition of its significance as the first public catalog of gravitational-wave transients, and recommendation for minor revision. We note that the report contains no specific major comments or criticisms requiring substantive changes.
Circularity Check
No significant circularity
full rationale
The paper is an observational catalog reporting detections and parameter estimates from LIGO/Virgo strain data using three independent search pipelines and standard Bayesian inference. Source properties and significances are computed directly from the data with explicit noise models and sensitivity estimates. Merger rates are inferred under explicitly stated assumptions of fixed population distributions and reported as 90% confidence intervals; these are conditioned inferences rather than quantities fitted by construction to the target rates. No load-bearing step reduces to a self-definition, a renamed fit, or a self-citation chain that renders the central claims tautological. The derivation chain is data-driven and self-contained against external benchmarks.
Axiom & Free-Parameter Ledger
free parameters (1)
- population distribution parameters
axioms (1)
- domain assumption Detector noise is stationary and Gaussian over the analysis segments
Lean theorems connected to this paper
-
Foundation/DimensionForcingdimension_forced unclear?
unclearRelation between the paper passage and the cited Recognition theorem.
gravitational waves from three binary black hole mergers were detected... seven binary black hole mergers... first detection of gravitational waves from a binary neutron star inspiral... merger rates at the 90% confidence intervals of 110 - 3840 Gpc^{-3} y^{-1} for binary neutron stars and 9.7 - 101 Gpc^{-3} y^{-1} for binary black holes assuming fixed population distributions
-
Foundation/PhiForcingphi_equation unclear?
unclearRelation between the paper passage and the cited Recognition theorem.
For all significant gravitational-wave events, we provide estimates of the source properties... using relativistic models of GWs from CBCs
What do these tags mean?
- matches
- The paper's claim is directly supported by a theorem in the formal canon.
- supports
- The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
- extends
- The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
- uses
- The paper appears to rely on the theorem as machinery.
- contradicts
- The paper's claim conflicts with a theorem or certificate in the canon.
- unclear
- Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.
Forward citations
Cited by 31 Pith papers
-
Constraints on the Primordial Black Hole Abundance using Pulsar Parameter Drifts
The first search for scalar-induced gravitational waves via pulsar parameter drifts yields f_PBH < 10^{-10} (95% CL) for PBH masses 0.3 to 4e4 solar masses, strongly disfavoring a primordial black hole origin for LVK ...
-
Testing the Kerr hypothesis beyond the quadrupole with GW241011
GW241011 data shows consistency with Kerr black holes for both quadrupole and octupole moments and delivers the first observational bounds on spin-induced octupole deviations.
-
Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions
The gwNRHME framework constructs a multi-modal non-spinning eccentric gravitational waveform surrogate by modulating quasi-circular models with universal eccentric functions, achieving median mismatches of ~9e-5 again...
-
Gravitational wave signal and noise response of an optically levitated sensor in a Fabry-P\'erot cavity
A general relativistic derivation of gravitational wave response in an optically levitated cavity sensor reveals position-dependent strain sensitivity and suppressed input-mirror noise coupling.
-
GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run
LIGO and Virgo detected 39 compact binary coalescence events in O3a, including 13 new ones, with black hole binaries up to 150 solar masses and the first significantly asymmetric mass ratios.
-
Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework
A unified confluent HeunC framework with hybrid connection-coefficient computation and adaptive bi-power quadrature yields relative errors of order 10^{-11} and 2-10x speedups over existing packages for total radiativ...
-
Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework
A unified confluent HeunC framework computes gravitational-wave fluxes from generic Kerr orbits with 10^{-11} relative errors and speedups of 3-60x over existing packages for low- and high-order modes.
-
Non-Parametric Equation of State Reveals Non-Conformal Behavior Beyond Neutron Star Densities
Non-parametric EOS construction shows non-conformal behavior with evidence for soft quark matter and a hadron-quark phase transition in massive neutron star cores.
-
Implications of the LISA stochastic signal from eccentric stellar mass black hole binaries in vacuum
High initial eccentricities in stellar-mass black hole binaries produce a stochastic gravitational wave background distinguishable by LISA from quasi-circular models, enabling upper bounds on eccentricity and separati...
-
Gravitational Waves from a Black Hole Falling Radially into a Thin-Shell Traversable Wormhole
Analytic gravitational waveforms from radial test-particle infall into a thin-shell traversable wormhole exhibit a characteristic pulse-gap structure from repeated throat crossings and lie within reach of ground-based...
-
Normalizing flows for density estimation in multi-detector gravitational-wave searches
Normalizing flows replace binned histograms for estimating multi-detector signal parameters in PyCBC, slashing storage by three orders of magnitude with under 0.05% sensitivity loss and up to 6.55% gains in specific cases.
-
Boson star-black hole binaries: initial data and head-on collisions
A one-body conformal-factor correction stabilizes boson star-black hole initial data, enabling gravitational-wave analysis that shows higher multipoles can discriminate mixed mergers from pure black-hole binaries.
-
Fast neural network surrogate for multimodal effective-one-body gravitational waveforms from generically precessing compact binaries
Neural network surrogate approximates precessing compact binary gravitational waveforms up to 1000x faster than the base EOB model with validated accuracy.
-
Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects
pyEFPEHM extends prior PN models to include higher-order quasi-circular phasing, generalized precession solutions, and eccentric corrections up to 1PN in selected multipoles for eccentric precessing binaries with matt...
-
Second-Generation Mass Peak in the Gravitational-Wave Population as a Probe of Globular Clusters
Dynamical formation in globular clusters produces a robust second black-hole mass peak at ~70 solar masses from second-generation mergers when the first-generation spectrum is truncated by pair-instability supernovae.
-
Computationally efficient models for the dominant and sub-dominant harmonic modes of precessing binary black holes
IMRPhenomXPHM is a new computationally efficient phenomenological model for precessing binary black hole gravitational-wave signals that incorporates higher-order modes via twisting-up maps from non-precessing waveforms.
-
The Impact of Spin Priors on Parameterized Tests of General Relativity
Spin prior choices propagate into tests of GR via the 1.5PN deviation parameter δφ̂3 in a non-trivial, event-dependent way, with stronger effects for short-inspiral events and partial degeneracy with χ_eff when the de...
-
Ringdown Analysis of GW250114 with Orthonormal Modes
Orthonormal QNM analysis of GW250114 raises the significance of the first overtone of the ℓ=m=2 mode from 82.5% to 99.9% and detects no significant deviation from Kerr predictions.
-
Purely Quadratic Non-Gaussianity from Tachyonic Instability: Primordial Black Holes and Scalar-Induced Gravitational Waves
Purely quadratic non-Gaussianity from tachyonic instability allows narrow curvature spectra to exponentially suppress primordial black hole overproduction via correlation coefficient ρ approaching -1 while retaining s...
-
Black Hole-Boson Star Binaries: Gravitational Wave Signals and Tidal Disruption
Numerical simulations of black hole-boson star binaries show that scalar self-interactions can suppress tidal disruption while radiative efficiency depends on the chosen potential.
-
Probing Kerr Symmetry Breaking with LISA Extreme-Mass-Ratio Inspirals
LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.
-
Inference of recoil kicks from binary black hole mergers up to GWTC--4 and their astrophysical implications
Recoil kicks are inferred for GWTC-4 binary black hole events with values up to nearly 1000 km/s for some, yielding retention probabilities of 1-5% in globular clusters and 70-100% in elliptical galaxies.
-
A Horizon Study for Cosmic Explorer: Science, Observatories, and Community
Cosmic Explorer is described as a next-generation gravitational-wave observatory aiming for tenfold sensitivity improvement over Advanced LIGO to observe signals from the edge of the observable universe at z~100.
-
Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog
No evidence for deviations from general relativity is found in LIGO-Virgo binary black hole events, with improved constraints on waveform parameters, graviton mass, and ringdown properties.
-
Gravitational-wave astronomy requires population-informed parameter estimation
Population-informed hierarchical parameter estimation is required for unbiased astrophysical interpretation of gravitational-wave events rather than using standard individual posteriors with reference priors.
-
Not too close! Evaluating the impact of the baseline on the localization of binary black holes by next-generation gravitational-wave detectors
Baselines of 8-11 ms light travel time for two CE detectors provide a reasonable compromise for BBH sky localization, with third detectors eliminating multimodality for most or all events.
-
GW190711_030756 and GW200114_020818: astrophysical interpretation of two asymmetric binary black hole mergers in the IAS catalog
Two asymmetric BBH mergers are characterized with mass ratios 0.35 and ≤0.20; one shows high spins, negative χ_eff, and strong precession, suggesting an emerging population of massive rapidly spinning systems.
-
Tests of General Relativity with GWTC-3
No evidence for physics beyond general relativity is found in the analysis of 15 GW events from GWTC-3, with consistency in residuals, PN parameters, and remnant properties.
-
Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies
The paper reviews cosmological tensions including the H0 and S8 discrepancies and explores new physics models that could explain them.
- Gravitational-wave constraints on the pair-instability mass gap and nuclear burning in massive stars
- Inferring the properties of a population of compact binaries in presence of selection effects
Reference graph
Works this paper leans on
-
[1]
J. Aasi et al. (LIGO Scientific Collaboration), Advanced LIGO, Classical Quantum Gravity 32, 074001 (2015)
work page 2015
-
[2]
F. Acernese et al. (Virgo Collaboration), Advanced Virgo: A Second-Generation Interferometric Gravitational Wave Detector, Classical Quantum Gravity 32, 024001 (2015)
work page 2015
-
[3]
A. H. Nitz, I. W. Harry, J. L. Willis, C. M. Biwer, D. A. Brown, L. P . Pekowsky, T. Dal Canton, A. R. Williamson, T. Dent, C. D. Capano, T. J. Massinger, A. K. Lenon, A. B. Nielsen, and M. Cabero, PyCBC Software, http://github .com/ligo-cbc/pycbc
-
[4]
S. A. Usman et al. , The PyCBC Search for Gravitational Waves from Compact Binary Coalescence , Classical Quantum Gravity 33, 215004 (2016)
work page 2016
-
[5]
S. Sachdev et al. , The GstLAL Search Analysis Methods for Compact Binary Mergers in Advanced LIGO ’s Second and Advanced Virgo ’s First Observing Runs , arXiv: 1901.08580
work page Pith review arXiv 1901
-
[6]
C. Messick et al. , Analysis Framework for the Prompt Discovery of Compact Binary Mergers in Gravitational- Wave Data , Phys. Rev. D 95, 042001 (2017)
work page 2017
-
[7]
S. Klimenko et al., Method for Detection and Reconstruction of Gravitational Wave Transients with Networks of Ad- vanced Detectors, Phys. Rev. D 93, 042004 (2016)
work page 2016
-
[8]
A. Krolak and B. F. Schutz, Coalescing Binaries —Probe of the Universe , Gen. Relativ. Gravit. 19, 1163 (1987)
work page 1987
- [9]
-
[10]
The event GW151012 was previously referred to as L VT151012. Here, we retire the LVT nomenclature; all candidate events with an estimated FAR of less than 1 per 30 days and a probability of > 0.5 of being of astrophysi- cal origin [see Eq. (10) for the definition] are henceforth denoted with the GW prefix. All other candidates are referred to as marginal
-
[11]
B. P . Abbott et al. (VIRGO, LIGO Scientific Collabora- tion), GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2 , Phys. Rev. Lett. 118, 221101 (2017)
work page 2017
-
[12]
B. P . Abbott et al. (Virgo, LIGO Scientific Collaboration), GW170814: A Three-Detector Observation of Gravita- tional Waves from a Binary Black Hole Coalescence , Phys. Rev. Lett. 119, 141101 (2017)
work page 2017
-
[13]
B. P . Abbott et al. (Virgo, LIGO Scientific Collaboration), GW170608: Observation of a 19-Solar-Mass Binary Black Hole Coalescence , Astrophys. J. 851, L35 (2017)
work page 2017
-
[14]
B. P . Abbott et al. (Virgo, LIGO Scientific Collaboration), GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral, Phys. Rev. Lett. 119, 161101 (2017)
work page 2017
-
[15]
B. F. Schutz, Networks of Gravitational Wave Detectors and Three Figures of Merit , Classical Quantum Gravity 28, 125023 (2011)
work page 2011
-
[16]
S. Fairhurst, Source Localization with an Advanced Gravitational Wave Detector Network , Classical Quantum Gravity 28, 105021 (2011)
work page 2011
-
[17]
B. P . Abbott et al. [GROND, SALT Group, OzGrav, DFN, INTEGRAL, Virgo, Insight-Hxmt, MAXI Team, Fermi- LA T, J-GEM, RA TIR, IceCube, CAASTRO, LW A, ePES- STO, GRAWITA, RIMAS, SKA South Africa/MeerKA T, H.E.S.S., 1M2H Team, IKI-GW Follow-up, Fermi GBM, Pi of Sky, DWF (Deeper Wider Faster Program), Dark Energy Survey, MASTER, AstroSat Cadmium Zinc Telluride...
work page 2017
-
[18]
B. P . Abbott et al. (LIGO Scientific, Virgo Collaboration), Low-Latency Gravitational Wave Alerts for Multi- Messenger Astronomy during the Second Advanced LIGO and Virgo Observing Run , Astrophys. J. 875, 161 (2019)
work page 2019
-
[19]
P . Ajith et al. , Inspiral-Merger-Ringdown Waveforms for Black-Hole Binaries with Non-Precessing Spins , Phys. Rev. Lett. 106, 241101 (2011)
work page 2011
-
[20]
L. Santamaría et al. , Matching Post-Newtonian and Numerical Relativity Waveforms: Systematic Errors and a New Phenomenological Model for Non-Precessing Black Hole Binaries , Phys. Rev. D 82, 064016 (2010)
work page 2010
-
[21]
M. Hannam, P . Schmidt, A. Boh´ e, L. Haegel, S. Husa, F. Ohme, G. Pratten, and M. Pürrer, Simple Model of Complete Precessing Black-Hole-Binary Gravitational Waveforms, Phys. Rev. Lett. 113, 151101 (2014) . GWTC-1: A GRA VITA TIONAL-W A VE TRANSIENT CA TALOG… PHYS. REV . X 9, 031040 (2019) 031040-35
work page 2014
-
[22]
S. Khan, S. Husa, M. Hannam, F. Ohme, M. Pürrer, X. J. Forteza, and A. Boh´ e, Frequency-Domain Gravitational Waves from Nonprecessing Black-Hole Binaries. II. A Phenomenological Model for the Advanced Detector Era , Phys. Rev. D 93, 044007 (2016)
work page 2016
-
[23]
Y . Pan, A. Buonanno, A. Taracchini, L. E. Kidder, A. H. Mrou´e, H. P . Pfeiffer, M. A. Scheel, and B. Szilágyi, Inspiral-Merger-Ringdown Waveforms of Spinning, Pre- cessing Black-Hole Binaries in the Effective-One-Body Formalism, Phys. Rev. D 89, 084006 (2014)
work page 2014
-
[24]
A. Taracchini et al., Effective-One-Body Model for Black- Hole Binaries with Generic Mass Ratios and Spins , Phys. Rev. D 89, 061502 (2014)
work page 2014
-
[25]
A. Boh´e et al., An Improved Effective-One-Body Model of Spinning, Nonprecessing Binary Black Holes for the Era of Gravitational-Wave Astrophysics with Advanced Detec- tors, Phys. Rev. D 95, 044028 (2017)
work page 2017
- [26]
-
[27]
T. Hinderer et al. , Effects of Neutron-Star Dynamic Tides on Gravitational Waveforms within the Effective-One- Body Approach , Phys. Rev. Lett. 116, 181101 (2016)
work page 2016
-
[28]
T. Dietrich et al. , Matter Imprints in Waveform Models for Neutron Star Binaries: Tidal and Self-Spin Effects , arXiv:1804.02235
-
[29]
A. Nagar et al. , Time-Domain Effective-One-Body Gravi- tational Waveforms for Coalescing Compact Binaries with Nonprecessing Spins, Tides and Self-Spin Effects , Phys. Rev. D 98, 104052 (2018)
work page 2018
-
[30]
L. Blanchet, B. R. Iyer, C. M. Will, and A. G. Wiseman, Gravitational Wave Forms from Inspiralling Compact Binaries to Second Post-Newtonian Order , Classical Quantum Gravity 13, 575 (1996)
work page 1996
- [31]
-
[32]
L. Blanchet, T. Damour, G. Esposito-Farese, and B. R. Iyer, Dimensional Regularization of the Third Post- Newtonian Gravitational Wave Generation from Two Point Masses , Phys. Rev. D 71, 124004 (2005)
work page 2005
-
[33]
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)
work page 2009
-
[34]
L. Blanchet, Gravitational Radiation from Post- Newtonian Sources and Inspiralling Compact Binaries , Living Rev. Relativity 17, 2 (2014)
work page 2014
-
[35]
A. Buonanno and T. Damour, Effective One-Body Ap- proach to General Relativistic Two-Body Dynamics , Phys. Rev. D 59, 084006 (1999)
work page 1999
-
[36]
A. Buonanno and T. Damour, Transition from Inspiral to Plunge in Binary Black Hole Coalescences , Phys. Rev. D 62, 064015 (2000)
work page 2000
- [37]
-
[38]
T. Damour and A. Nagar, An Improved Analytical Description of Inspiralling and Coalescing Black-Hole Binaries, Phys. Rev. D 79, 081503 (2009)
work page 2009
-
[39]
E. Barausse and A. Buonanno, An Improved Effective- One-Body Hamiltonian for Spinning Black-Hole Binaries , Phys. Rev. D 81, 084024 (2010)
work page 2010
-
[40]
T. Damour and A. Nagar, The Effective-One-Body Approach to the General Relativistic Two Body Problem , Lect. Notes Phys. 905, 273 (2016)
work page 2016
-
[41]
Pretorius, Evolution of Binary Black Hole Spacetimes , Phys
F. Pretorius, Evolution of Binary Black Hole Spacetimes , Phys. Rev. Lett. 95, 121101 (2005)
work page 2005
-
[42]
M. Campanelli, C. O. Lousto, P . Marronetti, and Y . Zlochower, Accurate Evolutions of Orbiting Black-Hole Binaries without Excision , Phys. Rev. Lett. 96, 111101 (2006)
work page 2006
-
[43]
J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, and J. van Meter, Gravitational Wave Extraction from an Inspiraling Configuration of Merging Black Holes , Phys. Rev. Lett. 96, 111102 (2006)
work page 2006
-
[44]
A. H. Mroue et al. , Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy, Phys. Rev. Lett. 111, 241104 (2013)
work page 2013
-
[45]
S. Husa, S. Khan, M. Hannam, M. Pürrer, F. Ohme, X. J. Forteza, and A. Boh´ e, Frequency-Domain Gravitational Waves from Nonprecessing Black-Hole Binaries. I. New Numerical Waveforms and Anatomy of the Signal , Phys. Rev. D 93, 044006 (2016)
work page 2016
-
[46]
T. Chu, H. Fong, P . Kumar, H. P . Pfeiffer, M. Boyle, D. A. Hemberger, L. E. Kidder, M. A. Scheel, and B. Szilagyi, On the Accuracy and Precision of Numerical Waveforms: Effect of Waveform Extraction Methodology , Classical Quantum Gravity 33, 165001 (2016)
work page 2016
- [47]
-
[48]
J. C. Driggers et al. (LIGO Scientific Collaboration), Improving Astrophysical Parameter Estimation via Offline Noise Subtraction for Advanced LIGO , Phys. Rev. D 99, 042001 (2019)
work page 2019
-
[49]
N. J. Cornish and T. B. L ittenberg, BayesWave: Baye- sian Inference for Gravitational Wave Bursts and Instrument Glitches , Classical Quantum Gravity 32, 135012 (2015)
work page 2015
-
[50]
T. B. Littenberg and N. J. Cornish, Bayesian Inference for Spectral Estimation of Gravitational Wave Detector Noise , Phys. Rev. D 91, 084034 (2015)
work page 2015
- [51]
-
[52]
LIGO Scientific Collaboration, Virgo Collaboration, GWTC-1, https://doi.org/10.7935/82H3-HH23
-
[53]
LIGO Scientific Collaboration, Virgo Collaboration, Gravitational Wave Open Science Center, https://www .gw-openscience.org
-
[54]
B. P . Abbott et al. (Virgo, LIGO Scientific Collaboration), GW150914: The Advanced LIGO Detectors in the Era of First Discoveries , Phys. Rev. Lett. 116, 131103 (2016) . B. P . ABBOTT et al. PHYS. REV . X 9, 031040 (2019) 031040-36
work page 2016
-
[55]
B. P . Abbott et al. , Sensitivity of the Advanced LIGO Detectors at the Beginning of Gravitational Wave Astronomy, Phys. Rev. D 93, 112004 (2016) ; 97, 059901(A) (2018)
work page 2016
- [56]
-
[57]
Interferometer performance is commonly reduced to a single scalar number that quantifies the distance to which a single instrument could detect a 1.4 M⊙ þ 1.4 M⊙ BNS merger, averaged over the sky location and orientation, with an average SNR of 8 [62,63]
- [58]
-
[59]
L. S. Finn and D. F. Chernoff, Observing Binary Inspiral in Gravitational Radiation: One Interferometer, Phys. Rev. D 47, 2198 (1993)
work page 1993
-
[60]
C. Cahillane et al. (LIGO Scientific Collaboration), Cal- ibration Uncertainty for Advanced LIGO ’s First and Second Observing Runs , Phys. Rev. D 96, 102001 (2017)
work page 2017
-
[61]
A. Viets et al., Reconstructing the Calibrated Strain Signal in the Advanced LIGO Detectors , Classical Quantum Gravity 35, 095015 (2018)
work page 2018
- [62]
-
[63]
F. Acernese et al. (Virgo Collaboration), Calibration of Advanced Virgo and Reconstruction of the Gravitational Wave Signal hðtÞ during the Observing Run O2 , Classical Quantum Gravity 35, 205004 (2018)
work page 2018
-
[64]
B. P . Abbott et al. (Virgo, LIGO Scientific Collaboration), Effects of Data Quality Vetoes on a Search for Compact Binary Coalescences in Advanced LIGO ’s First Observing Run, Classical Quantum Gravity 35, 065010 (2018)
work page 2018
-
[65]
T. Dal Canton, A. P . Lundgren, and A. B. Nielsen, Impact of Precession on Aligned-Spin Searches for Neutron-Star – Black-Hole Binaries , Phys. Rev. D 91, 062010 (2015)
work page 2015
- [66]
-
[67]
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)
work page 2005
-
[68]
A. H. Nitz, Distinguishing Short Duration Noise Transi- ents in LIGO Data to Improve the PyCBC Search for Gravitational Waves from High Mass Binary Black Hole Mergers, Classical Quantum Gravity 35, 035016 (2018)
work page 2018
-
[69]
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)
work page 2017
-
[70]
This statement is true of almost all analysis periods, but the last analysis period in O2 has a slightly shorter length of approximately 3.6 days
-
[71]
T. Dal Canton and I. Harry, Designing a Template Bank to Observe Compact Binary Coalescences in Advanced LIGO’s Second Observing Run , arXiv:1705.01845
-
[72]
M. Pürrer, Frequency Domain Reduced Order Model of Aligned-Spin Effective-One-Body Waveforms with Generic Mass-Ratios and Spins , Phys. Rev. D 93, 064041 (2016)
work page 2016
-
[73]
M. Pürrer, Frequency Domain Reduced Order Models for Gravitational Waves from Aligned-Spin Compact Bina- ries, Classical Quantum Gravity 31, 195010 (2014)
work page 2014
- [74]
-
[75]
LIGO Scientific Collaboration, Virgo Collaboration, LAL- Suite, https://git.ligo.org/lscsoft/lalsuite
-
[76]
G. Faye, S. Marsat, L. Blanchet, and B. R. Iyer, The Third and a Half Post-Newtonian Gravitational Wave Quadru- pole Mode for Quasi-Circular Inspiralling Compact Bina- ries, Classical Quantum Gravity 29, 175004 (2012)
work page 2012
-
[77]
As a reminder, GstLAL analyzes data from three interfer- ometers, so the light travel time depends on the specific interferometers involved in any particular candidate
- [78]
-
[79]
C. Hanna et al. , Fast Evaluation of Multi-Detector Con- sistency for Real-Time Gravitational Wave Searches , arXiv:1901.02227
-
[80]
D. Mukherjee et al. , The GstLAL Template Bank for Spinning Compact Binary Mergers in the Second Obser- vation Run of Advanced LIGO and Virgo , arXiv:1812 .05121
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.