{"work":{"id":"29d52a5a-6fd3-471b-8fec-d17c29cf9026","openalex_id":null,"doi":null,"arxiv_id":"1408.3978","raw_key":null,"title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","authors":null,"authors_text":"F. Acernese, M. Agathos, K. Agatsuma, D. Aisa, N. Allemandou, A. Allocca","year":2014,"venue":"gr-qc","abstract":"Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this paper we describe the main features of the Advanced Virgo detector and outline the status of the construction.","external_url":"https://arxiv.org/abs/1408.3978","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-07-04T19:40:06.434742+00:00","pith_arxiv_id":"1408.3978","created_at":"2026-05-09T02:57:49.786037+00:00","updated_at":"2026-07-04T19:40:06.434742+00:00","title_quality_ok":true,"display_title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","render_title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector"},"hub":{"state":{"work_id":"29d52a5a-6fd3-471b-8fec-d17c29cf9026","tier":"super_hub","tier_reason":"100+ Pith inbound or 10,000+ external citations","pith_inbound_count":110,"external_cited_by_count":null,"distinct_field_count":8,"first_pith_cited_at":"2019-03-11T17:43:43+00:00","last_pith_cited_at":"2026-07-01T18:34:19+00:00","author_build_status":"needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-08-22T14:19:24.507358+00:00","tier_text":"super_hub"},"tier":"super_hub","role_counts":[{"context_role":"background","n":40},{"context_role":"dataset","n":2},{"context_role":"method","n":2},{"context_role":"other","n":1}],"polarity_counts":[{"context_polarity":"background","n":38},{"context_polarity":"unclear","n":3},{"context_polarity":"use_dataset","n":2},{"context_polarity":"use_method","n":2}],"runs":{"ask_index":{"job_type":"ask_index","status":"succeeded","result":{"title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","claims":[{"claim_text":"Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this pa","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"latter two events, the evidence for eccentricity is ambiguous, with different degrees of support from different waveforms. Consistent with previous work, we find conclusions obtained about GW200129 can be sensitive to analysis settings, as expected, given the nonstationary noise present. I. INTRODUCTION Since the discovery of GW150914 095045 by the Ad- vanced LIGO [1] and Virgo [2] detectors, now joined by KAGRA [3], the first four observing runs (referred to as O1, O2, O3, and O4) of the LIGO-V","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"LIGO Laboratory which is a major facility fully funded by the NSF. REFERENCES [1] B. P. Abbottet al.(LIGO Scientific, Virgo), \"Observation of Gravitational Waves from a Binary Black Hole Merger,\" Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] J. Aasiet al.(LIGO Scientific), \"Advanced LIGO,\" Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [3] F. Acerneseet al.(Virgo), \"Advanced Virgo: a second- generation interferometric gravitational wave detector,\" Class. 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Acernese et al.,Advanced Virgo: a second-generation interferometric gravitational wave detector,Class. Quant. Grav.32(2015) 024001 [1408.3978]. [3] KAGRA collaboration, T. Akutsu et al.,Overview of KAGRA: Detector design and construction history,PTEP2021(2021) 05A101 [2005.","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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, The As- trophysical Journal 946, 59 (2023), arXiv:2112.06878 [astro- ph.HE]. [11] J. Aasi et al. (LIGO Scientific), Advanced LIGO, Class. Quant. Grav. 32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [12] F. Acernese et al. (VIRGO), Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. Quant. 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[1] Gregory M. Harry (LIGO Scientific), \"Advanced LIGO: The next generation of gravitational wave detectors,\" Class. Quant. Grav.27, 084006 (2010). [2] F. Acerneseet al.(VIRGO), \"Advanced Virgo: a second- generation interferometric gravitational wave detector,\" Class. Quant. Grav.32, 024001 (2015), arXiv:1408.3978 [gr-qc]. [3] T. Akutsuet al.(KAGRA), \"Overview of KAGRA: Detector design and construction history,\" PTEP2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]. [4] B. P. Abbottet al.(LIGO Scientific, Virgo), \"GWTC-1: A","citing_arxiv_id":"2604.07388"},{"n":1,"role":"method","polarity":"use_method","paper_title":"Tests of General Relativity with GWTC-3","primary_cat":"gr-qc","context_text":"the (2,2)-mode at the peak of the amplitude as defined in the model SEOBNRv4 [185]. We introduce the following parametric deviations to gravitational-wave inspiral phasing: {δ ˆφ−2, δˆφ0, δˆφ1, δˆφ2, δˆφ3, δˆφ4, δˆφ5l, δˆφ6, δˆφ6l, δˆφ7} , (5) where each δ ˆφi represents the fractional deviation from the GR PN coefficient at thei/2-th PN order, following the parametriza- tion adopted in previous analyses [7, 9, 10, 188, 189]. The sub- script l is used to denote coefficients of logarithmic-in- f terms. We do not present bounds for the 2.5PN non-logarithmic term, as this is degenerate with the coalescence phase, as can be seen from Eq. (4). As predicted in GR, the coefficients correspond- ing to −1PN and 0.5PN are identically zero, so we parametrize δ ˆφ−2 and δ ˆφ1 as absolute deviations, with a prefactor equal to","citing_arxiv_id":"2112.06861"}]},"error":null,"updated_at":"2026-05-16T23:19:24.194628+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":"2026-05-16T23:19:24.132653+00:00"},"role_polarity":{"job_type":"role_polarity","status":"succeeded","result":{"title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","claims":[{"claim_text":"Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this pa","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"latter two events, the evidence for eccentricity is ambiguous, with different degrees of support from different waveforms. Consistent with previous work, we find conclusions obtained about GW200129 can be sensitive to analysis settings, as expected, given the nonstationary noise present. I. INTRODUCTION Since the discovery of GW150914 095045 by the Ad- vanced LIGO [1] and Virgo [2] detectors, now joined by KAGRA [3], the first four observing runs (referred to as O1, O2, O3, and O4) of the LIGO-V","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"LIGO Laboratory which is a major facility fully funded by the NSF. REFERENCES [1] B. P. Abbottet al.(LIGO Scientific, Virgo), \"Observation of Gravitational Waves from a Binary Black Hole Merger,\" Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] J. Aasiet al.(LIGO Scientific), \"Advanced LIGO,\" Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [3] F. Acerneseet al.(Virgo), \"Advanced Virgo: a second- generation interferometric gravitational wave detector,\" Class. Quant","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"These considerations should be useful to inform the development of the XG detector network. I. INTRODUCTION In the past decade, the observation of the gravitational- wave (GW) signal emitted by compact binary coalescences (CBCs) gave us a new tool to study the Universe. With more than 200 event candidates observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) detectors, the GWs give us insight into the demography of masses, redshifts, and spins of compact object binaries [4, 5], the nature of ","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"struction's flatter amplitude profile does not track the data as closely asNRSur7dq4. [1] LIGO Scientificcollaboration, J. Aasi et al.,Advanced LIGO, Class. Quant. Grav.32(2015) 074001 [1411.4547]. [2] VIRGO collaboration, F. Acernese et al.,Advanced Virgo: a second-generation interferometric gravitational wave detector,Class. Quant. Grav.32(2015) 024001 [1408.3978]. [3] KAGRA collaboration, T. Akutsu et al.,Overview of KAGRA: Detector design and construction history,PTEP2021(2021) 05A101 [2005.","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"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, The As- trophysical Journal 946, 59 (2023), arXiv:2112.06878 [astro- ph.HE]. [11] J. Aasi et al. (LIGO Scientific), Advanced LIGO, Class. Quant. Grav. 32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [12] F. Acernese et al. (VIRGO), Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. Quant. Grav. 32, 024001 ","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"A Review: Noise spectra of interferometer and pulsar timing experiments 30 A.1 Formalism 31 A.2 Transfer functions 36 A.3 Detector noise power spectra 40 A.4 Strain noise power spectra 43 1 Introduction Since the celebrated first direct detection ofgravitational waves (GWs) in September 2015 [3], the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO) [4, 5] and the Advanced Virgo (aVirgo) experiment [6] have observed a multitude of GW events [7, 8]. One of the signals recorded d","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks Advanced Virgo: a 2nd generation interferometric gravitational wave detector because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (39 contexts).","role_counts":[{"n":39,"context_role":"background"},{"n":2,"context_role":"method"},{"n":1,"context_role":"dataset"},{"n":1,"context_role":"other"}]},"error":null,"updated_at":"2026-07-03T00:03:12.764117+00:00"},"summary_claims":{"job_type":"summary_claims","status":"succeeded","result":{"title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","claims":[{"claim_text":"Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this pa","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"LIGO Laboratory which is a major facility fully funded by the NSF. REFERENCES [1] B. P. Abbottet al.(LIGO Scientific, Virgo), \"Observation of Gravitational Waves from a Binary Black Hole Merger,\" Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] J. Aasiet al.(LIGO Scientific), \"Advanced LIGO,\" Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [3] F. Acerneseet al.(Virgo), \"Advanced Virgo: a second- generation interferometric gravitational wave detector,\" Class. Quant","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"These considerations should be useful to inform the development of the XG detector network. I. INTRODUCTION In the past decade, the observation of the gravitational- wave (GW) signal emitted by compact binary coalescences (CBCs) gave us a new tool to study the Universe. With more than 200 event candidates observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) detectors, the GWs give us insight into the demography of masses, redshifts, and spins of compact object binaries [4, 5], the nature of ","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"18080 [gr-qc]. [2] A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, (2025), arXiv:2508.18082 [gr-qc]. 6 [3] J. Aasiet al.(LIGO Scientific), Advanced LIGO, Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [4] F. Acerneseet al.(VIRGO), Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. Quant. Grav.32, 024","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"source properties from there derived are naturally suited to astrophysical interpretation and catalog statistics, such as identification of exceptional events from previous and ongoing observing runs. Using the latest LIGO-Virgo-KAGRA data, we thus demonstrate that population inference is not optional to interpret gravitational-wave observations. Pitfalls of parameter estimation-Gravitational- wave (GW) signals observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) interferometers are used to ","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]. [6] R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]. [7] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [8] J. Aasiet al.(LIGO Scientific), Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [9] F. Acerneseet al.(VIRGO), Class. Quant. Grav.32, 024001 (2015), arXiv:1408.3978 [gr-qc]. [10] T. Akutsuet al.(KAGRA), PTEP2021, 05","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"reduces parameter degeneracies and accelerates compu- tations [76]. In this paper, we apply this approach to the event GW250114 082203, henceforth GW250114 [15]. This event was detected by the LIGO detectors [77] on January 14, 2025, and has the largest network signal-to- noise ratio (SNR) to date, with a value of approximately 80 [15, 16]. At the time of this event, the Virgo [78] and KAGRA [79] detectors were not in operation. Ref- erence [15] reports an inspiral-merger-ringdown (IMR) analysis","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks Advanced Virgo: a 2nd generation interferometric gravitational wave detector because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (17 contexts).","role_counts":[{"n":17,"context_role":"background"},{"n":1,"context_role":"dataset"},{"n":1,"context_role":"method"}]},"error":null,"updated_at":"2026-05-16T23:19:19.201833+00:00"}},"summary":{"title":"Advanced Virgo: a 2nd generation interferometric gravitational wave detector","claims":[{"claim_text":"Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this pa","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"LIGO Laboratory which is a major facility fully funded by the NSF. REFERENCES [1] B. P. Abbottet al.(LIGO Scientific, Virgo), \"Observation of Gravitational Waves from a Binary Black Hole Merger,\" Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] J. Aasiet al.(LIGO Scientific), \"Advanced LIGO,\" Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [3] F. Acerneseet al.(Virgo), \"Advanced Virgo: a second- generation interferometric gravitational wave detector,\" Class. Quant","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"These considerations should be useful to inform the development of the XG detector network. I. INTRODUCTION In the past decade, the observation of the gravitational- wave (GW) signal emitted by compact binary coalescences (CBCs) gave us a new tool to study the Universe. With more than 200 event candidates observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) detectors, the GWs give us insight into the demography of masses, redshifts, and spins of compact object binaries [4, 5], the nature of ","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"18080 [gr-qc]. [2] A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, (2025), arXiv:2508.18082 [gr-qc]. 6 [3] J. Aasiet al.(LIGO Scientific), Advanced LIGO, Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [4] F. Acerneseet al.(VIRGO), Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. Quant. Grav.32, 024","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"source properties from there derived are naturally suited to astrophysical interpretation and catalog statistics, such as identification of exceptional events from previous and ongoing observing runs. Using the latest LIGO-Virgo-KAGRA data, we thus demonstrate that population inference is not optional to interpret gravitational-wave observations. Pitfalls of parameter estimation-Gravitational- wave (GW) signals observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) interferometers are used to ","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]. [6] R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]. [7] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [8] J. Aasiet al.(LIGO Scientific), Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [9] F. Acerneseet al.(VIRGO), Class. Quant. Grav.32, 024001 (2015), arXiv:1408.3978 [gr-qc]. [10] T. Akutsuet al.(KAGRA), PTEP2021, 05","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"reduces parameter degeneracies and accelerates compu- tations [76]. In this paper, we apply this approach to the event GW250114 082203, henceforth GW250114 [15]. This event was detected by the LIGO detectors [77] on January 14, 2025, and has the largest network signal-to- noise ratio (SNR) to date, with a value of approximately 80 [15, 16]. At the time of this event, the Virgo [78] and KAGRA [79] detectors were not in operation. Ref- erence [15] reports an inspiral-merger-ringdown (IMR) analysis","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks Advanced Virgo: a 2nd generation interferometric gravitational wave detector because it crossed a citation-hub threshold. Current citing contexts most often use it as background evidence (17 contexts).","role_counts":[{"n":17,"context_role":"background"},{"n":1,"context_role":"dataset"},{"n":1,"context_role":"method"}]},"graph":{"co_cited":[{"title":"Advanced LIGO","work_id":"b93186e6-8d0a-440a-aa48-9de6dbff57b9","shared_citers":42},{"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":27},{"title":"Akutsuet al.(KAGRA), Overview of KAGRA: Detector design and construction history, PTEP2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]","work_id":"5d6cbaec-f994-4631-bca0-649752990e3b","shared_citers":26},{"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":25},{"title":"GWTC-4.0: Population Properties of 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Run","work_id":"7410f8dd-43ce-418e-a2fe-baea0cf36999","shared_citers":17},{"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":16},{"title":"dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evidences","work_id":"838bbbf0-e03a-4893-a204-1a830384f3ff","shared_citers":16},{"title":"Abbottet al.(LIGO Scientific, Virgo), GW190521: A Bi- nary Black Hole Merger with a Total Mass of 150M ⊙, Phys","work_id":"b7256b8f-454f-4ef5-bf26-277f8874afda","shared_citers":14},{"title":"Abbottet al.(LIGO Scientific, Virgo), Properties and As- trophysical Implications of the 150 M ⊙ Binary Black Hole Merger GW190521, Astrophys","work_id":"197bfdeb-5c5e-45d7-ad75-4a5480282ac5","shared_citers":13},{"title":"GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\\odot}$","work_id":"acb0e78d-b098-4d33-a93c-a75b3583cf54","shared_citers":13},{"title":"Post-Newtonian Theory for Gravitational Waves","work_id":"6cb2442c-e284-4ded-a540-4da7a2454980","shared_citers":13},{"title":"Surrogate models for precessing binary black hole simulations with unequal masses","work_id":"6cb84ac5-4771-456b-9c60-97cc2e74d509","shared_citers":13},{"title":"The PyCBC search for gravitational waves from compact binary coalescence","work_id":"f9a7a128-751f-4159-9767-e3259c17a4b0","shared_citers":13},{"title":"Ade et al","work_id":"a36b7348-19d6-4af7-9627-ad462b9f2c8a","shared_citers":12},{"title":"GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","work_id":"38dc3e43-0988-49cb-9c1d-d4ee3fffc8bb","shared_citers":12},{"title":"GWTC-4.0: Methods for Identifying and Characterizing Gravitational-wave Transients","work_id":"642e86b9-e3ac-4047-aca4-761cb674b6d2","shared_citers":11},{"title":"Klimenkoet al., Method for detection and reconstruction of gravitational wave transients with networks of advanced de- tectors, Phys","work_id":"39037c90-cfbe-43e6-996c-5b6a5666beb9","shared_citers":11},{"title":"Messicket al., Analysis Framework for the Prompt Discov- ery of Compact Binary Mergers in Gravitational-wave Data, Phys","work_id":"00c44cda-7e7f-4ac4-9098-4f9bf94d9096","shared_citers":11},{"title":"Tests of general relativity with GW150914","work_id":"6360cb89-3e23-4c10-b265-09130bfbf688","shared_citers":11}],"time_series":[{"n":2,"year":2019},{"n":3,"year":2020},{"n":2,"year":2021},{"n":7,"year":2025},{"n":33,"year":2026}],"dependency_candidates":[{"n":1,"role":"dataset","polarity":"use_dataset","paper_title":"GW190711_030756 and GW200114_020818: astrophysical interpretation of two asymmetric binary black hole mergers in the IAS catalog","primary_cat":"astro-ph.HE","context_text":"Recherche Scientifique (CNRS), the Italian Istituto Nazionale di Fisica Nucleare (INFN) and the Dutch Nikhef, with contribu- tions by institutions from Belgium, Germany, Greece, Hungary, Ireland, Japan, Monaco, Poland, Portugal, Spain. [1] Gregory M. Harry (LIGO Scientific), \"Advanced LIGO: The next generation of gravitational wave detectors,\" Class. Quant. Grav.27, 084006 (2010). [2] F. Acerneseet al.(VIRGO), \"Advanced Virgo: a second- generation interferometric gravitational wave detector,\" Class. Quant. Grav.32, 024001 (2015), arXiv:1408.3978 [gr-qc]. [3] T. Akutsuet al.(KAGRA), \"Overview of KAGRA: Detector design and construction history,\" PTEP2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]. [4] B. P. Abbottet al.(LIGO Scientific, Virgo), \"GWTC-1: A","citing_arxiv_id":"2604.07388"},{"n":1,"role":"method","polarity":"use_method","paper_title":"Tests of General Relativity with GWTC-3","primary_cat":"gr-qc","context_text":"the (2,2)-mode at the peak of the amplitude as defined in the model SEOBNRv4 [185]. We introduce the following parametric deviations to gravitational-wave inspiral phasing: {δ ˆφ−2, δˆφ0, δˆφ1, δˆφ2, δˆφ3, δˆφ4, δˆφ5l, δˆφ6, δˆφ6l, δˆφ7} , (5) where each δ ˆφi represents the fractional deviation from the GR PN coefficient at thei/2-th PN order, following the parametriza- tion adopted in previous analyses [7, 9, 10, 188, 189]. The sub- script l is used to denote coefficients of logarithmic-in- f terms. We do not present bounds for the 2.5PN non-logarithmic term, as this is degenerate with the coalescence phase, as can be seen from Eq. (4). As predicted in GR, the coefficients correspond- ing to −1PN and 0.5PN are identically zero, so we parametrize δ ˆφ−2 and δ ˆφ1 as absolute deviations, with a prefactor equal to","citing_arxiv_id":"2112.06861"}]},"authors":[{"id":"8f436737-5794-4f32-8c68-2c9c0d34e925","orcid":null,"display_name":"A. Allocca","source":"manual","import_confidence":0.72},{"id":"5e52c5d8-29ee-44f9-a7fe-8fadbcca9ae6","orcid":null,"display_name":"D. Aisa","source":"manual","import_confidence":0.72},{"id":"59d922b0-a777-47ce-97f2-3d652ee7e69e","orcid":null,"display_name":"F. Acernese","source":"manual","import_confidence":0.72},{"id":"bb7aa49c-506c-44d5-8aee-6dd959de3dee","orcid":null,"display_name":"K. Agatsuma","source":"manual","import_confidence":0.72},{"id":"7e72841c-3af4-4f41-b87c-d1ea27cf55a8","orcid":null,"display_name":"M. Agathos","source":"manual","import_confidence":0.72},{"id":"e4fcd247-5afb-46c9-964a-bb970be876b0","orcid":null,"display_name":"N. Allemandou","source":"manual","import_confidence":0.72}]}}