{"work":{"id":"a1a21d1d-87a3-4fbe-be6f-efe2ea2acb33","openalex_id":null,"doi":null,"arxiv_id":"2112.06861","raw_key":null,"title":"Tests of General Relativity with GWTC-3","authors":null,"authors_text":"The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration: R. Abbott, H. Abe, F. Acernese, K. Ackley","year":2021,"venue":"gr-qc","abstract":"The ever-increasing number of detections of gravitational waves (GWs) from compact binaries by the Advanced LIGO and Advanced Virgo detectors allows us to perform ever-more sensitive tests of general relativity (GR) in the dynamical and strong-field regime of gravity. We perform a suite of tests of GR using the compact binary signals observed during the second half of the third observing run of those detectors. We restrict our analysis to the 15 confident signals that have false alarm rates $\\leq 10^{-3}\\, {\\rm yr}^{-1}$. In addition to signals consistent with binary black hole (BH) mergers, the new events include GW200115_042309, a signal consistent with a neutron star--BH merger. We find the residual power, after subtracting the best fit waveform from the data for each event, to be consistent with the detector noise. Additionally, we find all the post-Newtonian deformation coefficients to be consistent with the predictions from GR, with an improvement by a factor of ~2 in the -1PN parameter. We also find that the spin-induced quadrupole moments of the binary BH constituents are consistent with those of Kerr BHs in GR. We find no evidence for dispersion of GWs, non-GR modes of polarization, or post-merger echoes in the events that were analyzed. We update the bound on the mass of the graviton, at 90% credibility, to $m_g \\leq 2.42 \\times 10^{-23} \\mathrm{eV}/c^2$. The final mass and final spin as inferred from the pre-merger and post-merger parts of the waveform are consistent with each other. The studies of the properties of the remnant BHs, including deviations of the quasi-normal mode frequencies and damping times, show consistency with the predictions of GR. In addition to considering signals individually, we also combine results from the catalog of GW signals to calculate more precise population constraints. We find no evidence in support of physics beyond GR.","external_url":"https://arxiv.org/abs/2112.06861","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-05-23T23:58:38.807102+00:00","pith_arxiv_id":"2112.06861","created_at":"2026-05-08T23:14:23.454995+00:00","updated_at":"2026-05-23T23:58:38.807102+00:00","title_quality_ok":true,"display_title":"Tests of General Relativity with GWTC-3","render_title":"Tests of General Relativity with GWTC-3"},"hub":{"state":{"work_id":"a1a21d1d-87a3-4fbe-be6f-efe2ea2acb33","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":67,"external_cited_by_count":null,"distinct_field_count":7,"first_pith_cited_at":"2023-03-28T12:29:33+00:00","last_pith_cited_at":"2026-05-20T18:51:46+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-05-27T08:17:34.048063+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"background","n":32},{"context_role":"method","n":4},{"context_role":"baseline","n":1},{"context_role":"dataset","n":1}],"polarity_counts":[{"context_polarity":"background","n":30},{"context_polarity":"use_method","n":3},{"context_polarity":"support","n":2},{"context_polarity":"baseline","n":1},{"context_polarity":"unclear","n":1},{"context_polarity":"use_dataset","n":1}],"runs":{"context_extract":{"job_type":"context_extract","status":"succeeded","result":{"enqueued_papers":25},"error":null,"updated_at":"2026-05-18T16:31:14.778504+00:00"},"graph_features":{"job_type":"graph_features","status":"succeeded","result":{"co_cited":[{"title":"Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog","work_id":"62bb917e-cb23-4dd7-970e-02affb9488c2","shared_citers":25},{"title":"Tests of general relativity with GW150914","work_id":"6360cb89-3e23-4c10-b265-09130bfbf688","shared_citers":22},{"title":"GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run","work_id":"da52a8d9-11a6-46c6-a2f5-89dab8381497","shared_citers":21},{"title":"Observation of Gravitational Waves from a Binary Black Hole Merger","work_id":"ab878228-151c-4a29-8026-a4308b076d30","shared_citers":21},{"title":"GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run","work_id":"373a2c61-2309-4528-87c8-9053657b5ebd","shared_citers":20},{"title":"Tests of General Relativity with the Binary Black Hole Signals from the LIGO-Virgo Catalog GWTC-1","work_id":"f83ceb1b-d07d-4ffc-bdc6-8f2da0284397","shared_citers":19},{"title":"Computationally efficient models for the dominant and sub-dominant harmonic modes of precessing binary black holes","work_id":"00f3c2bc-d169-42df-be45-172745f646cd","shared_citers":17},{"title":"Bilby: A user-friendly Bayesian inference library for gravitational-wave astronomy","work_id":"d639e2d8-7766-4408-a78b-d70b05a88b81","shared_citers":16},{"title":"Advanced LIGO","work_id":"b93186e6-8d0a-440a-aa48-9de6dbff57b9","shared_citers":15},{"title":"Black Hole Spectroscopy and Tests of General Relativity with GW250114","work_id":"dc4b2f4a-8133-4076-a219-13310060c8bd","shared_citers":15},{"title":"Black hole spectroscopy: from theory to experiment","work_id":"d5c07d13-a0ab-4c80-9fcd-dbbfcd03378c","shared_citers":15},{"title":"GW250114: testing Hawking's area law and the Kerr nature of black holes","work_id":"ae0e7d73-d72a-4821-b5bb-33144bbb87ba","shared_citers":15},{"title":"Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO","work_id":"de7f174c-dbb7-4870-b03c-7faf70dce4e9","shared_citers":14},{"title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","work_id":"29d52a5a-6fd3-471b-8fec-d17c29cf9026","shared_citers":13},{"title":"GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","work_id":"7410f8dd-43ce-418e-a2fe-baea0cf36999","shared_citers":13},{"title":"dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evidences","work_id":"838bbbf0-e03a-4893-a204-1a830384f3ff","shared_citers":12},{"title":"GWTC-4.0: Population Properties of Merging Compact Binaries","work_id":"3cc938ec-4259-4f1a-86fc-6864781ec8d3","shared_citers":12},{"title":"Testing the no-hair theorem with GW150914","work_id":"2bddf9bb-186a-45da-84bf-96e24c09de85","shared_citers":11},{"title":"Black Hole Spectroscopy: Testing General Relativity through Gravitational Wave Observations","work_id":"9ade9377-de34-4ad4-b0be-2e076e71952f","shared_citers":10},{"title":"GWTC-4.0: Tests of General Relativity. III. Tests of the Remnants","work_id":"37a861b4-515e-496b-ab30-e13e9f018a80","shared_citers":10},{"title":"GWTC-4.0: Tests of General Relativity. II. Parameterized Tests","work_id":"3ad285f2-e253-4387-842a-198e2b1d5481","shared_citers":10},{"title":"GWTC-4.0: Tests of General Relativity. I. Overview and General Tests","work_id":"e3141b37-9c4c-4db8-93d6-57fceff0c23d","shared_citers":10},{"title":"On gravitational-wave spectroscopy of massive black holes with the space interferometer LISA","work_id":"cfe4ac61-803e-48f3-b347-aba10239f146","shared_citers":10},{"title":"Quasinormal modes of black holes and black branes","work_id":"51775bcb-14dc-4eec-8c8c-179fd9588810","shared_citers":10}],"time_series":[{"n":1,"year":2023},{"n":15,"year":2025},{"n":35,"year":2026}],"dependency_candidates":[{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"Improved Constraints on Non-Kerr Deviations from Binary Black Hole Inspirals Using GWTC-4 Data","primary_cat":"gr-qc","context_text":"arXiv:1602.03838 [gr-qc]. [3] B. P. Abbottet al., Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [4] B. P. Abbottet al., Phys. Rev. D100, 104036 (2019), arXiv:1903.04467 [gr-qc]. [5] R. Abbottet al., Phys. Rev. D103, 122002 (2021), arXiv:2010.14529 [gr-qc]. [6] R. Abbottet al., Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr-qc]. [7] A. G. Abacet al., (2026), arXiv:2603.19019 [gr-qc]. [8] A. G. Abacet al., (2026), arXiv:2603.19020 [gr-qc]. [9] A. G. Abacet al., (2026), arXiv:2603.19021 [gr-qc]. [10] N. V. Krishnendu and F. Ohme, Universe7, 497 (2021), arXiv:2201.05418 [gr-qc]. [11] B. P. Abbottet al., Phys. Rev. Lett.116, 221101 (2016), [Erratum: Phys.Rev.Lett. 121, 129902 (2018)],","citing_arxiv_id":"2604.15965"},{"n":1,"role":"method","polarity":"use_method","paper_title":"Robust parameter inference for Taiji via time-frequency contrastive learning and normalizing flows","primary_cat":"gr-qc","context_text":"responding interferometric observable. We sample these parameters over the rangesdv∈[1×10 −15,1×10 −13], τ1 ∈[2.0,60.0], andτ 2 ∈[2.0,60.0], which define the family of short-duration transient artifacts considered in this work [55, 117]. During training, the glitch ampli- tude is further rescaled such that the glitch signal-to- noise ratio spans the range [8,32], thereby exposing the inference network to a broad set of moderate contami- nation levels. For evaluation, we additionally consider substantially stronger glitch realizations, with test cases extending to glitch SNRs as high as 103, in order to assess the extrapolative robustness of the proposed framework under extreme non-stationary contamination.","citing_arxiv_id":"2604.13867"},{"n":1,"role":"baseline","polarity":"baseline","paper_title":"Novel ringdown tests of general relativity with black hole greybody factors","primary_cat":"gr-qc","context_text":"129,111102(2022),arXiv:2201.00822[gr-qc]. [27] M. Isi and W. M. Farr, Phys. Rev. Lett.131, 169001 (2023), arXiv:2310.13869 [astro-ph.HE]. 6 [28] G. Carullo, R. Cotesta, E. Berti, and V. Cardoso, Phys. Rev.Lett.131,169002(2023),arXiv:2310.20625[gr-qc]. [29] R. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. D 103, 122002 (2021), arXiv:2010.14529 [gr-qc]. [30] R. Abbottet al.(LIGO Scientific, VIRGO, KAGRA), (2021), arXiv:2112.06861 [gr-qc]. [31] A. Guptaet al., (2024), 10.21468/SciPostPhysComm- Rep.5, arXiv:2405.02197 [gr-qc]. [32] A. Dhani, S. H. Völkel, A. Buonanno, H. Estelles, J. Gair, H. P. Pfeiffer, L. Pompili, and A. Toubiana, Phys. Rev. X15, 031036 (2025), arXiv:2404.05811 [gr- qc]. [33] J. Calderón Bustillo, P.","citing_arxiv_id":"2604.11895"},{"n":1,"role":"method","polarity":"use_method","paper_title":"GW250114: testing Hawking's area law and the Kerr nature of black holes","primary_cat":"gr-qc","context_text":", Analysis Framework for the Prompt Discov- ery of Compact Binary Mergers in Gravitational-wave Data, Phys. Rev. D95, 042001 (2017), arXiv:1604.04324 [astro- ph.IM]. [82] S. Sachdevet al., The GstLAL Search Analysis Methods for Compact Binary Mergers in Advanced LIGO's Sec- ond and Advanced Virgo's First Observing Runs (2019), arXiv:1901.08580 [gr-qc]. [83] C. Hannaet al., Fast evaluation of multidetector consistency for real-time gravitational wave searches, Phys. Rev. D101, 022003 (2020), arXiv:1901.02227 [gr-qc]. [84] K. Cannonet al., GstLAL: A software framework for grav- itational wave discovery, SoftwareX14, 100680 (2021), arXiv:2010.05082 [astro-ph.IM]. [85] L. Tsukadaet al., Improved ranking statistics of the GstLAL","citing_arxiv_id":"2509.08054"}]},"error":null,"updated_at":"2026-05-18T16:31:14.870480+00:00"},"identity_refresh":{"job_type":"identity_refresh","status":"succeeded","result":{"items":[{"title":"Qwen3 Technical Report","outcome":"unchanged","work_id":"25a4e30c-1232-48e7-9925-02fa12ba7c9e","resolver":"local_arxiv","confidence":0.98,"old_work_id":"25a4e30c-1232-48e7-9925-02fa12ba7c9e"}],"counts":{"fixed":0,"merged":0,"unchanged":1,"quarantined":0,"needs_external_resolution":0},"errors":[],"attempted":1},"error":null,"updated_at":"2026-05-18T16:31:11.798866+00:00"},"summary_claims":{"job_type":"summary_claims","status":"succeeded","result":{"title":"Tests of General Relativity with GWTC-3","claims":[{"claim_text":"The ever-increasing number of detections of gravitational waves (GWs) from compact binaries by the Advanced LIGO and Advanced Virgo detectors allows us to perform ever-more sensitive tests of general relativity (GR) in the dynamical and strong-field regime of gravity. We perform a suite of tests of GR using the compact binary signals observed during the second half of the third observing run of those detectors. We restrict our analysis to the 15 confident signals that have false alarm rates $\\leq 10^{-3}\\, {\\rm yr}^{-1}$. In addition to signals consistent with binary black hole (BH) mergers, t","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"the number of BBH observations by the LIGO-Virgo- KAGRA (LVK) collaboration [2-5] has steadily increased, reaching∼200detections over four observing runs [6]. These observations have provided unprecedented insights ∗ aravichandran@umassd.edu into the properties of black holes and the dynamics of their mergers, which have been crucial for testing general relativity (GR) in the strong-field regime [7] and un- derstanding the astrophysical processes that lead to the formation of BBHs [8]. In most s","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"making GW astronomy an increasingly promising avenue for the study of open problems in fundamental physics and cosmology. A central question that GW astronomy aims to address is theblack hole hypothesis- whether all the astrophysical objects believed to be BHs are indeed well-modeled by the classical BHs of general relativity. To date, all obser- vations of GW events [8], as well as interferometric ob- servations of BH environments using the Event Horizon Telescope [9, 10] are consistent with cl","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"Lopez-Aleman, \"Black Hole Spectroscopy: Testing General Relativity through Gravitational Wave Observations,\" Class. Quant. Grav.21, 787-804 (2004) [arXiv:gr-qc/0309007]. [9] E. Berti, V. Cardoso, and C. M. Will, \"On Gravitational-Wave Spectroscopy of Massive Black Holes with the Space Interferometer LISA,\" Phys. Rev. D73, 064030 (2006) [arXiv:gr-qc/0512160]. [10] R. Abbottet al.(LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration), \"Tests of General Relativity with GWTC-3","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"2975 [gr-qc] . [5] O. Trivedi, A. Gurrola, and R. J. Scherrer, (2026), arXiv:2603.04375 [gr-qc] . [6] B. P. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. Lett.116, 221101 (2016), [Erratum: Phys.Rev.Lett. 121, 129902 (2018)], arXiv:1602.03841 [gr-qc] . [7] R. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. D103, 122002 (2021), arXiv:2010.14529 [gr-qc] . [8] R. Abbott et al. (LIGO Scientific, VIRGO, KAGRA), (2021), arXiv:2112.06861 [gr-qc] . [9] S. 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D103, 122002 (2021), arXiv:2010.14529 [gr-qc]. [6] R. Abbottet al., Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr-qc]. [7] A. G. Abacet al., (2026), arXiv:2603.19019 [gr-qc]. [8] A. G. Abacet al., (2026), arXiv:2603.19020 [gr-qc]. [9] A. G. Abacet al., (2026), arXiv:","claim_type":"dataset","confidence":0.9,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks Tests of General Relativity with GWTC-3 because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (26 contexts).","role_counts":[{"n":26,"context_role":"background"},{"n":2,"context_role":"method"},{"n":1,"context_role":"baseline"},{"n":1,"context_role":"dataset"}]},"error":null,"updated_at":"2026-05-18T16:31:06.900941+00:00"}},"summary":{"title":"Tests of General Relativity with GWTC-3","claims":[{"claim_text":"The ever-increasing number of detections of gravitational waves (GWs) from compact binaries by the Advanced LIGO and Advanced Virgo detectors allows us to perform ever-more sensitive tests of general relativity (GR) in the dynamical and strong-field regime of gravity. We perform a suite of tests of GR using the compact binary signals observed during the second half of the third observing run of those detectors. We restrict our analysis to the 15 confident signals that have false alarm rates $\\leq 10^{-3}\\, {\\rm yr}^{-1}$. In addition to signals consistent with binary black hole (BH) mergers, t","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"the number of BBH observations by the LIGO-Virgo- KAGRA (LVK) collaboration [2-5] has steadily increased, reaching∼200detections over four observing runs [6]. These observations have provided unprecedented insights ∗ aravichandran@umassd.edu into the properties of black holes and the dynamics of their mergers, which have been crucial for testing general relativity (GR) in the strong-field regime [7] and un- derstanding the astrophysical processes that lead to the formation of BBHs [8]. In most s","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"making GW astronomy an increasingly promising avenue for the study of open problems in fundamental physics and cosmology. A central question that GW astronomy aims to address is theblack hole hypothesis- whether all the astrophysical objects believed to be BHs are indeed well-modeled by the classical BHs of general relativity. To date, all obser- vations of GW events [8], as well as interferometric ob- servations of BH environments using the Event Horizon Telescope [9, 10] are consistent with cl","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"Lopez-Aleman, \"Black Hole Spectroscopy: Testing General Relativity through Gravitational Wave Observations,\" Class. Quant. Grav.21, 787-804 (2004) [arXiv:gr-qc/0309007]. [9] E. Berti, V. Cardoso, and C. M. Will, \"On Gravitational-Wave Spectroscopy of Massive Black Holes with the Space Interferometer LISA,\" Phys. Rev. D73, 064030 (2006) [arXiv:gr-qc/0512160]. [10] R. Abbottet al.(LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration), \"Tests of General Relativity with GWTC-3","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"2975 [gr-qc] . [5] O. Trivedi, A. Gurrola, and R. J. Scherrer, (2026), arXiv:2603.04375 [gr-qc] . [6] B. P. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. Lett.116, 221101 (2016), [Erratum: Phys.Rev.Lett. 121, 129902 (2018)], arXiv:1602.03841 [gr-qc] . [7] R. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. D103, 122002 (2021), arXiv:2010.14529 [gr-qc] . [8] R. Abbott et al. (LIGO Scientific, VIRGO, KAGRA), (2021), arXiv:2112.06861 [gr-qc] . [9] S. Chandrasekhar, The mathematical theory of","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"of the Fourth LIGO-Virgo-KAGRA Observing Run,\" (2025), 2508.18082. [9] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. D100, 104036 (2019), arXiv:1903.04467 [gr-qc]. [10] R. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. X 11, 021053 (2021), arXiv:2010.14527 [gr-qc]. [11] R. Abbottet al.(LIGO Scientific, VIRGO, KAGRA), Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr- qc]. [12] G. F. Giudice, M. McCullough, and A. Urbano, JCAP 1610, 001 (2016), arXiv:1605.01209 [hep-ph]. [13] V. Car","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"arXiv:1602.03838 [gr-qc]. [3] B. P. Abbottet al., Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [4] B. P. Abbottet al., Phys. Rev. D100, 104036 (2019), arXiv:1903.04467 [gr-qc]. [5] R. Abbottet al., Phys. Rev. D103, 122002 (2021), arXiv:2010.14529 [gr-qc]. [6] R. Abbottet al., Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr-qc]. [7] A. G. Abacet al., (2026), arXiv:2603.19019 [gr-qc]. [8] A. G. Abacet al., (2026), arXiv:2603.19020 [gr-qc]. [9] A. G. 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Abbottet al., Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr-qc]. [7] A. G. Abacet al., (2026), arXiv:2603.19019 [gr-qc]. [8] A. G. Abacet al., (2026), arXiv:2603.19020 [gr-qc]. [9] A. G. Abacet al., (2026), arXiv:2603.19021 [gr-qc]. [10] N. V. Krishnendu and F. Ohme, Universe7, 497 (2021), arXiv:2201.05418 [gr-qc]. [11] B. P. Abbottet al., Phys. Rev. Lett.116, 221101 (2016), [Erratum: Phys.Rev.Lett. 121, 129902 (2018)],","citing_arxiv_id":"2604.15965"},{"n":1,"role":"method","polarity":"use_method","paper_title":"Robust parameter inference for Taiji via time-frequency contrastive learning and normalizing flows","primary_cat":"gr-qc","context_text":"responding interferometric observable. We sample these parameters over the rangesdv∈[1×10 −15,1×10 −13], τ1 ∈[2.0,60.0], andτ 2 ∈[2.0,60.0], which define the family of short-duration transient artifacts considered in this work [55, 117]. 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