{"total":45,"items":[{"citing_arxiv_id":"2605.21599","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: stellar population catalogue for galaxies in GOODS-N and GOODS-S","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:04:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JADES DR5 delivers a public catalog of Bayesian-inferred stellar masses, SFRs, SFHs, dust, metallicities, and AGN contributions for ~500k galaxies via Prospector with an evolving SFMS prior.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20060","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting Dark Sector field theory with phantom crossing","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T16:18:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"An interacting dark sector model with Yukawa-coupled fermionic DM and Born-Infeld tachyonic scalar produces recent double phantom crossing in effective w_DE, fits DESI+Planck+SN data, and predicts ultralight DM mass of order 1.9e-3 eV under naturalness assumptions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18742","ref_index":80,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A universal framework to identify eccentric binary mergers: GW200105 case study","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T17:58:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A reference-frequency-independent detection statistic for eccentric binary mergers is introduced and applied to GW200105, yielding ln B ≤ 0.9 in favor of the eccentric aligned-spin model over the quasi-circular precessing model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16994","ref_index":73,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Determination of the best dark matter profile for the Milky Way with Gaia DR3 using Bayesian Model Comparison","primary_cat":"astro-ph.GA","submitted_at":"2026-05-16T13:42:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian comparison of Gaia DR3 rotation curves favors the Einasto dark matter profile over NFW, prefers cored over cuspy profiles, and finds MOND variants provide poorer fits than the best dark matter models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16505","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Feedback driven interactions between dark and luminous matter to explain tight galaxy scaling relations","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"NIHAO simulations reproduce the Rd-r0 relation and its mild evolution from z=2 to z=0 through stellar feedback without dark matter modifications.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15749","ref_index":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on primordial black holes from the first part of LIGO-Virgo-KAGRA fourth observing run","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T09:07:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LIGO-Virgo-KAGRA O4a data yields the strongest constraints on primordial black hole abundance for 0.6-100 solar masses, with resolvable mergers dominating the limits and no compelling evidence for a PBH contribution in joint fits with astrophysical black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15263","ref_index":69,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the quenching of LRD X-ray emission by both Compton-thick gas and high accretion rates","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LRDs require Compton-thick gas at moderate metallicity plus high accretion rates producing weak X-rays to explain their non-detection, implying they are not chemically pristine.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16425","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Polarization Birefringence and Waveform Systematics in GW231123","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T15:23:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Analysis of GW231123 with IMRPhenomXPHM, IMRPhenomXO4a and NRSur7dq4 yields no waveform-independent evidence for polarization birefringence, with 90% upper limits on the derived coefficient of 0.378, 0.097 and 0.273 respectively.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11703","ref_index":166,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","primary_cat":"gr-qc","submitted_at":"2026-05-12T07:58:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"The first informative astrophysical calibration of gravitational-wave detectors is reported using GW240925 and GW250207.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"spiral software pipeline [51-54], with the MBTA pipeline [60, 61], the PyCBC package [157-159] and thecWB pack- ages [49, 50, 160-162]. Estimates of the noise spectra and glitch models, as well as tests of residuals, were obtained using BayesWa ve[163-165]. Signal parameter estimation was performed with the Bilbylibrary [70, 71] using the Dynestynested-sampling package [166]. SEOBNRv5PHM waveforms used in parameter estimation were generated us- ingpySEOBNR [167]. PESummarywas used to postpro- cess and collate parameter-estimation results [168]. Tests of GR were performed with the FTI [116], TIGER [118- 120] andpSEOBNR [126-130] tests implemented in Bil- byTGR [169], as well as with the QNMRF [131-134] and ringdown[135-137] pipelines."},{"citing_arxiv_id":"2605.04579","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The Impact of Spin Priors on Parameterized Tests of General Relativity","primary_cat":"gr-qc","submitted_at":"2026-05-06T07:30:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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 deviation is included.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"(iv) using the modified spin prior with the inclusion of the deviation parameterδ ˆϕ3. All analyses are performed using thebilbyframework (v2.7.1) together withbilby pipe (v1.7.0) for parameter estimation [36, 37]. Tests of general relativity are implemented viabilbytgr (v0.2). Waveform generation and detector response are handled bylalsuite(v7.26.1), and pos- terior sampling is carried out using the nested samplerdynesty(v3.0.0) [38, 39]. The waveform model employed in this work is the precessing waveform approximantIMRPhenomXPHM[40]. Using publicly available posterior samples and posterior samples obtained from newly per- formed parameter estimation runs, we obtain Fig. 1. As shown in Fig. 1, the violin plots compare the posterior distributions under two spin priors. We find thatχ effremains relatively stable (see"},{"citing_arxiv_id":"2605.03021","ref_index":37,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Closing the knowledge gap in semileptonic $B\\rightarrow X_c\\ell\\nu$ decays","primary_cat":"hep-ph","submitted_at":"2026-05-04T18:00:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The unmeasured fraction of inclusive semileptonic B to charm decays is dominated by final states without D mesons, likely from baryons and Ds mesons.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"for B+ decays (top) and B0 decays (bottom) for the two con- sidered fit scenarios in which the components are determined independently for B+ and B0 decays (orange) and assuming isospin symmetry (blue). The inner and outer ellipses corre- spond to the 1 and 2σcontours, respectively. The figures were generated with the plotting framework of EOS v1.0.19 [ 37, 38]. are in good agreement with each other as demonstrated in Fig. 1. Our results yield a non-vanishing branching ratio into Ds or baryonic final states at the 99% confidence level, indicating a significant Xc component that does not re- sult in final states involving D mesons. The resulting branching fraction can be compared to upper limits on B→DsXℓνand B→ΛcXℓνdecays."},{"citing_arxiv_id":"2604.15965","ref_index":47,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Improved Constraints on Non-Kerr Deviations from Binary Black Hole Inspirals Using GWTC-4 Data","primary_cat":"gr-qc","submitted_at":"2026-04-17T11:29:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Bayesian constraints from GWTC-4 binary black hole inspirals show Johannsen metric deformation parameters α13 and ε3 consistent with zero, supporting the Kerr hypothesis.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"of deformation parameters in a parametrized metric ap- proach. Our results show that including GWTC-4 events yields tighter constraints on individual deformation pa- rameters. The results remain consistent with the predic- tions of GR, with no statistically significant evidence of deviations from the Kerr metric. Fig. 2 compares new and old GW constraints on α13 with electromagnetic constraints [47] and updates Fig. 5.13 in Ref. [48]. Every error bar shows the 3-σ constraint inferred from the source/event indicated by the label. We use different colors for the constraints inferred with different techniques. The error bars in green show the most precise and accurate measurements ofα 13 from stellar-mass black holes with X-ray reflec- tion spectroscopy [49, 50]."},{"citing_arxiv_id":"2604.15885","ref_index":72,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravitational-wave astronomy requires population-informed parameter estimation","primary_cat":"gr-qc","submitted_at":"2026-04-17T09:31:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Population-informed hierarchical parameter estimation is required for unbiased astrophysical interpretation of gravitational-wave events rather than using standard individual posteriors with reference priors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"09442 [gr-qc]. [68] M. Mould, github.com/mdmould/gwax, doi.org/10.5281/zenodo.12770127 (2026). [69] R. Essicket al., Phys. Rev. D112, 102001 (2025), arXiv:2508.10638 [gr-qc]. [70] V. Tiwari, Class. Quantum Grav.35, 145009 (2018), arXiv:1712.00482 [astro-ph.HE]. [71] G. Ashtonet al., Astrophys. J. Supp. S.241, 27 (2019), arXiv:1811.02042 [astro-ph.IM]. [72] J. S. Speagle, Mon. Not. R. Astron. Soc.493, 3132 (2020), arXiv:1904.02180 [astro-ph.IM]. [73] M. Fishbach, D. E. Holz, and W. M. Farr, Astrophys. J. Lett.863, L41 (2018), arXiv:1805.10270 [astro-ph.HE]. [74] P. A. R. Adeet al., Astron. Astrophys.594, A13 (2016), arXiv:1502.01589 [astro-ph.CO]. [75] V. De Renzis, F. Iacovelli, D. Gerosa, M. Mancar-"},{"citing_arxiv_id":"2604.14270","ref_index":105,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Fast neural network surrogate for multimodal effective-one-body gravitational waveforms from generically precessing compact binaries","primary_cat":"gr-qc","submitted_at":"2026-04-15T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Neural network surrogate approximates precessing compact binary gravitational waveforms up to 1000x faster than the base EOB model with validated accuracy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Speagle, dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evi- dences, Mon. Not. Roy. Astron. Soc.493, 3132 (2020), arXiv:1904.02180 [astro-ph.IM]. [104] 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]. [105] L. Santamariaet al., Matching post-Newtonian and numerical relativity waveforms: systematic errors and a new phenomenological model for non-precessing black hole binaries, Phys. Rev. D82, 064016 (2010), arXiv:1005.3306 [gr-qc]. [106] P. Schmidt, F. Ohme, and M. Hannam, Towards mod- els of gravitational waveforms from generic binaries II: Modelling precession effects with a single effective pre-"},{"citing_arxiv_id":"2604.13839","ref_index":33,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Basilic: An end-to-end pipeline for Bayesian burst inference and model classification in gravitational-wave data","primary_cat":"gr-qc","submitted_at":"2026-04-15T13:10:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Basilic is an end-to-end Bayesian pipeline for gravitational-wave burst inference and model classification, with a case study showing signal degeneracies between binary black hole mergers and cosmic strings.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"each hand-picked BBH parameter combination is simply a differentYAMLconfiguration file provided toBasilic, which alternatively can also be provided with parameter grids in a single setup file as well, the injection campaign is then automated and results aggregated. For repro- ducibility, we utilize 4 s segments, a sampling frequency of 2048 Hz and 600 live points with the nested sampler dynesty[33, 34]. Since our study focuses on combinations of BBH pa- rameters that resemble cosmic string cusps in general, our CSC prior is quite unconstrained, with the ampli- tude log-uniform in [10 −23,10 −18] and high frequency cutoff uniform in [25,512]. As for the sky localization, we assume the position of the BBH source in the sky to be known, to lower problem dimensionality, while we let"},{"citing_arxiv_id":"2604.12987","ref_index":125,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T17:22:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Node-based reconstruction of cosmic expansion prefers stronger deceleration at z≈1.7 than smooth DE EoS parametrizations, isolating z~1.5-2 as a window where the latter may compress localized kinematic features permitted by current data.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"history can be obtained straightforwardly by differenti- ating the interpolant for each posterior sample. In this way, uncertainties inE ′(z),H ′(z), andq(z) are prop- agated directly through the sampling procedure rather than reconstructed in a separate post-processing step. For parameter estimation and evidence evaluation, we use theSimpleMCcode [124], which employs the nested- sampling packagedynesty[125] to implement nested sampling [126]. Each run is performed with 500 live points and a convergence tolerance of 0.01. In the re- construction framework we adopt broad flat priorsH 0 ∈ [40,90] km s −1 Mpc−1,E i ∈[0.5,4.0]. These node lo- cations and priors are chosen to cover the redshift range directly probed by the late-time data while remaining ag-"},{"citing_arxiv_id":"2604.12587","ref_index":69,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Impact of the SNe Ia Magnitude Transition at 20 Mpc on Cosmological Parameter Estimation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T11:10:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A 0.19 mag step in supernova absolute magnitude at 20 Mpc improves data fit and increases the Hubble constant by 2% while leaving matter density and dark energy parameters stable.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the Pacific125, 306-312 (2013). [67] Joshua S Speagle, \"dynesty: a dynamic nested sam- pling package for estimating bayesian posteriors and evi- dences,\" Monthly Notices of the Royal Astronomical So- ciety493, 3132-3158 (2020). [68] Matt Visser, \"Jerk, snap and the cosmological equation 21 of state,\" Classical and Quantum Gravity21, 2603-2615 (2004). [69] Jun-Qing Xia, Vincenzo Vitagliano, Stefano Liberati, and Matteo Viel, \"Cosmography beyond standard candles and rulers,\" Physical Review D85(2012), 10.1103/physrevd.85.043520. [70] C' eline Catto¨ en and Matt Visser, \"The hubble series: con- vergence properties and redshift variables,\" Classical and Quantum Gravity24, 5985-5997 (2007). [71] Bill S."},{"citing_arxiv_id":"2604.11903","ref_index":144,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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 matter effects.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"stability and robustness of the waveform model. There- fore, performing PE provides a stringent and informative validation of the waveform model. Here, we perform PE usingbilby[140-142], em- ploying its implementation of thedynesty[143] nested sampling algorithm. To assess the PE performance of pyEFPEHMin a controlled setting, we perform zero-noise injections [144]. This approach avoids both the statis- tical fluctuations associated with specific noise realiza- tions and the additional uncertainty inherent in real- event analyses, for which the true source parameters are unknown. Synthetic signals are injected into the LIGO Hanford (H1), LIGO Livingston (L1), and Virgo detec- tors, assuming the LIGO A+ and Virgo AdV+ sensitivity"},{"citing_arxiv_id":"2604.11895","ref_index":121,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Novel ringdown tests of general relativity with black hole greybody factors","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GreyRing model based on greybody factors reproduces numerical relativity ringdown signals with mismatches of order 10^{-6} and enables a new post-merger consistency test of general relativity applied to GW250114.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Mateu-Lucena, and R. Jaume, Phys. Rev. D102, 064002 (2020), arXiv:2001.10914 [gr-qc]. [119] LIGO Scientific Collaboration, \"LIGO Algorithm Li- brary - LALSuite,\" free software (GPL) (2018). [120] LIGO Scientific Collaboration and Virgo Collaboration, Noise Curves for use in simulations pre-O4, Tech. Rep. T2200043-v3 (LIGO Document Control Center (DCC), 2022). [121] J. S. Speagle, Mon. Not. Roy. Astron. Soc.493, 3132 (2020), arXiv:1904.02180 [astro-ph.IM]. [122] M. H.-Y. Cheung, E. Berti, V. Baibhav, and R. Cotesta, Phys. Rev. D109, 044069 (2024), [Erratum: Phys.Rev.D 110, 049902 (2024), Erratum: Phys.Rev.D 112, 049901 (2025)], arXiv:2310.04489 [gr-qc]. [123] S. A. Usmanet al., Class. Quant. Grav.33, 215004 (2016), arXiv:1508."},{"citing_arxiv_id":"2604.09828","ref_index":53,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Testing the Kerr hypothesis beyond the quadrupole with GW241011","primary_cat":"gr-qc","submitted_at":"2026-04-10T18:58:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Colleoni, A. Vijaykumar, K. G. Arun, and C. K. Mishra, Phys. Rev. D109, 023016 (2024), arXiv:2311.05506 [gr-qc]. [50] G. Prattenet al., Phys. Rev. D103, 104056 (2021), arXiv:2004.06503 [gr-qc]. [51] G. Ashtonet al., Astrophys. J. Suppl.241, 27 (2019), arXiv:1811.02042 [astro-ph.IM]. [52] J. S. Speagle, MNRAS493, 3132 (2020), arXiv:1904.02180 [astro-ph.IM]. [53] I. M. Romero-Shawet al., Mon. Not. Roy. Astron. Soc. 499, 3295 (2020), arXiv:arXiv:2006.00714 [astro-ph.IM] [astro-ph.IM]. [54] F. D. Ryan, Phys. Rev. D.55, 6081 (1997). [55] N. Uchikata, S. Yoshida, and P. Pani, Phys. Rev.D94, 064015 (2016), arXiv:1607.03593 [gr-qc]. [56] A. G. Abacet al.(LIGO Scientific, Virgo, KAGRA), Astrophys. J. Lett.993, L21 (2025), arXiv:2510."},{"citing_arxiv_id":"2604.08179","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GW231123: False Massive Graviton Signatures from Unmodeled Point-Mass Lensing","primary_cat":"gr-qc","submitted_at":"2026-04-09T12:35:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Unmodeled point-mass lensing produces a spurious nonzero graviton mass posterior in GW231123 that vanishes when lensing is included in the analysis.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Ganguly, Phys. Rev. D110, 084009 (2024), arXiv:2311.08446 [gr-qc]. [36] J. Skilling, inBayesian Inference and Maximum Entropy Methods in Science and Engineering, Vol. 735 (2004) pp. 395-405. [37] C. M. Biwer, C. D. Capano, S. De, M. Cabero, D. A. Brown, A. H. Nitz, and V. Raymond, Publ. Astron. Soc. Pac.131, 024503 (2019), arXiv:1807.10312 [astro-ph.IM]. [38] J. S. Speagle, Mon. Not. R. Astron. Soc.493, 3132 (2020), arXiv:1904.02180 [astro-ph.IM]. [39] G. Ashton, M. H¨ ubner, P. D. Lasky, C. Talbot, K. Ackley, S. Biscoveanu, Q. Chu, A. Divakarla, P. J. Easter, B. Goncharov, F. Hernandez Vivanco, J. Harms, M. E. Lower, G. D. Meadors, D. Melchor, E. Payne, M. D. Pitkin, J. Powell, N. Sarin, R. J. E. Smith,"},{"citing_arxiv_id":"2604.07388","ref_index":74,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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","submitted_at":"2026-04-08T05:45:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"frequency cutoffs tofmin =20 Hz and fmax =512 Hz, respec- tively. For GW200114_020818, we set fmin =15 Hz. For NRSur7dq4, we use a reference frequency of fref =17 Hz. We adopt the same priors as those used in standard LVK analy- ses and in the GWTC-3 reanalysis employing NRSur7dq4 in Ref. [52]. For sampling, we use the nested sampling [ 73] al- gorithm dynesty [74]. All waveforms are generated using the LALSimulationpackage [75, 76]. To assess waveform systematics, we additionally ana- lyze both events using two other waveform approximants, IMRPhenomXPHM and IMRPhenomTPHM. For IMRPhenomTPHM, we choose a lower reference frequency of fref =10 Hz, as this model prefers a lower reference frequency for wave- form generation, whereas for IMRPhenomXPHM we adopt the"},{"citing_arxiv_id":"2604.06090","ref_index":110,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Posterior Predictive Checks for Gravitational-wave Populations: Limitations and Improvements","primary_cat":"gr-qc","submitted_at":"2026-04-07T17:03:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Maximum-likelihood-based posterior predictive checks detect model misspecification better than event-level versions for uncertain spin tilts, but current detector sensitivity limits their power; the Gaussian Component Spins model underpredicts high spin magnitudes and overpredicts anti-aligned tilts","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"dimensional posterior of binary parameters using theIMRPhenomXPHMwaveform model, with standard priors for all parameters. Posteriors were sampled stochastically using the implementation of the nested samplerDynesty[96] in the parameter-estimation codeBilby[97]. A network optimal SNR cut of 10 was performed on the samples to ensure consistency with the selection process [110]. We establish the following notation for hierarchical/population inference. The posterior on population-level param- eters Λ given a GW catalog ⃗d(also called the \"hyper-posterior\") is p(Λ| ⃗d) = L( ⃗d|Λ)π(Λ) p( ⃗d) ,(A1) where the data ⃗d={d i}are fromN obs independent events, and the population likelihood (or \"hierarchical likelihood\") is L( ⃗d|Λ)∝"},{"citing_arxiv_id":"2603.06010","ref_index":147,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Accelerated Time-domain Analysis for Gravitational Wave Astronomy","primary_cat":"gr-qc","submitted_at":"2026-03-06T08:07:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Presents a practical fully time-domain end-to-end likelihood for gravitational-wave inference with structured linear algebra and GPU acceleration.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ernment of India, under project no. RTI4001. This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation Facilities: EGO:Virgo, GEO600, Kamioka:KAGRA, LIGO Software: Plots were prepared with Matplotlib [145], waveforms were generated through LALSuite [101, 146]. NumPy [147], SciPy [148] were used for data pro- cessing in generating the figures and quantities in the manuscript. Bilby [50, 149, 150] and Dynesty [133, 151] for stochastic sampling with Bayesian Inference. The time domain code used was developed by the author, be- ginning with his PhD thesis.tdanalysisis expected to be released to the public domain soon, but is currently"},{"citing_arxiv_id":"2602.11282","ref_index":112,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Measurement prospects for the pair-instability mass cutoff with gravitational waves","primary_cat":"astro-ph.HE","submitted_at":"2026-02-11T19:00:22+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations show a 40-50 solar-mass black-hole cutoff is not guaranteed to be confidently recovered from GWTC-4-like catalogs, spurious detections are unlikely, and O4 data would reduce cutoff-mass uncertainty by at least 20 percent while yielding only a lower bound on the carbon-alpha reaction rate","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"hood and regularization thereof from Ref. [17], including estimation of survey sensitivity [91, 103] and use of PE samples [74, 92]; we limit the relative Monte Carlo uncer- tainty of the likelihood estimator due to finite sampling to a maximum of unity [103-107]. Inference is performed usinggwax[108], withDynesty[109] for nested sam- pling [110, 111] throughBilby[112]. The mass models are summarized in Table I. The parameters of our models and the Bayesian priors we use for analyses of both real and simulated GW catalogs are given in Table IV. Though Ref. [17] now finds dimensionless BH spin magnitudes are better modeled as independently and identically distributed (IID) according to truncated Gaussians, as in Ref."},{"citing_arxiv_id":"2601.14222","ref_index":146,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","primary_cat":"astro-ph.CO","submitted_at":"2026-01-20T18:32:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"E(z) (1 +w E),(52) PC4:w eff DE(z) =w E − \u0014 γ E(z) +µ \u0015 (1 +w E),(53) It is important to note thatw eff DE(0)<−1/3 is required to consistently account for the current cosmic acceleration. V. DATASETS AND METHODOLOGY In this work we make use ofSimpleMC[144] as the sampling code. We employ Nested Sampling [145] as im- plemented in thedynestyPython library [146], which also provides the Bayesian Evidence needed to compare the PC models against the ΛCDM andw 0waCDM base- lines. For most analyses we used 1024 live points and an accuracy of 0.01 (which serves as the convergence crite- rion for nested sampling), ensuring good precision in the estimation of the evidence and posterior distributions. For the joint analysisCC+SN+SH0ES+BAO+CMB, we instead"},{"citing_arxiv_id":"2601.13173","ref_index":92,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Plunge-Merger-Ringdown Tests of General Relativity with GW250114","primary_cat":"gr-qc","submitted_at":"2026-01-19T15:57:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GW250114 data constrains GR deviations in merger amplitude to 10% and frequency to 4% at 90% CL, with first bounds on the (4,4) mode frequency at 6%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.07908","ref_index":110,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Signatures of a subpopulation of hierarchical mergers in the GWTC-4 gravitational-wave dataset","primary_cat":"gr-qc","submitted_at":"2026-01-12T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GWTC-4 data show a transition to nearly all hierarchical mergers above 46 solar masses, with the hierarchical rate peaking at 15.7 solar masses, indicating mass-dependent substructure in black hole spins.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"89, 035007 (2017), arXiv:1709.03144 [nucl-ex]. [108] G. Costa, A. Bressan, M. Mapelli, P. Marigo, G. Iorio, and M. Spera, Mon. Not. Roy. Astron. Soc.501, 4514 (2021), arXiv:2010.02242 [astro-ph.SR]. [109] C. Plunkett, T. Callister, M. Zevin, and S. Vitale, The data supporting the results of this study will be made available upon publication. (2025). [110] J. S. Speagle, Mon. Not. Roy. Astron. Soc.493, 3132 (2020), arXiv:1904.02180 [astro-ph.IM]. [111] G. Ashtonet al., Astrophys. J. Suppl.241, 27 (2019), arXiv:1811.02042 [astro-ph.IM]. [112] I. Mandel, W. M. Farr, and J. R. Gair, Mon. Not. Roy. Astron. Soc.486, 1086 (2019), arXiv:1809.02063 [physics.data-an]. [113] S. Vitale, D. Gerosa, W. M. Farr, and S."},{"citing_arxiv_id":"2512.17214","ref_index":59,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pulsed radio emission from a Central Compact Object","primary_cat":"astro-ph.HE","submitted_at":"2025-12-19T03:54:03+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"The central compact object 1E 1207.4-5209 emits pulsed radio waves at its 0.4-second spin period, revealing it as a faint radio pulsar.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.09978","ref_index":84,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational-wave parameter estimation to the Moon and back: massive binaries and the case of GW231123","primary_cat":"gr-qc","submitted_at":"2025-12-10T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LGWA could observe more than one third of known binary black hole events, detect ~90 mergers per year, and measure chirp mass better than third-generation detectors for massive systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.16879","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Accelerating parameter estimation for parameterized tests of general relativity with gravitational-wave observations","primary_cat":"gr-qc","submitted_at":"2025-11-21T01:08:52+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Relative binning accelerates TIGER parameterized GR tests by factors of 10-100 while recovering unbiased posteriors on simulated signals and real events like GW150914.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.17967","ref_index":114,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Scalar fields around black hole binaries in LIGO-Virgo-KAGRA","primary_cat":"gr-qc","submitted_at":"2025-10-20T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Semi-analytic waveform model for scalar environments around black hole binaries is validated against numerical relativity and applied to LIGO-Virgo-KAGRA data to obtain upper limits on scalar densities with tentative evidence in GW190728.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"ried out a Bayesian analysis of selected LVK events to search for scalar field effects. We analyzed pub- licly available strain data from the GWTC-3 catalog re- leased by the LVK Collaboration [86-89, 110, 111] using the IMRPhenomXPHM_Scalar waveform model, performing Bayesian inference using theBilbypackage [112, 113], employing theDynestynested sampling algorithm [114]. In our model, environmental corrections to the waveform are implemented only in the inspiral stage; therefore, an- alyzing events with low inspiral SNR is expected to be uninformative. Thus, we employ the same event selection criteria that are used in the LVK parameterized tests of general relativity: (i) a false-alarm rate (FAR) smaller than10 −3 yr−1, and (ii) an inspiral SNR greater than"},{"citing_arxiv_id":"2510.04332","ref_index":147,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Biased parameter inference of eccentric, spin-precessing binary black holes","primary_cat":"gr-qc","submitted_at":"2025-10-05T19:29:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Eccentric BBH signals recovered with quasi-circular precessing models show biases in chirp mass and χ_p; Bayes factors favor eccentric aligned-spin models when both eccentricity and precession are present.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"formed on thesonicHPC at ICTS-TIFR. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants Np. PHY-0757058 and No. PHY- 0823459. We used the following software packages: LALSuite[141],PyCBC[142],bilby[126],NumPy[143], Matplotlib[144],Seaborn[145],jupyter[146], dynesty[147],corner[148]. This document has LIGO preprint numberLIGO-P2500606. Appendix A: Priors used for parameter estimation The priors on various parameters used for non- spinning, aligned-spin, and precessing-spin analyses are listed in Table III. Parameter Prior Range M Uniform in component masses 5 - 50M ⊙ q Uniform in component masses 1 - 5 1 - 15a dL Uniform radius 100 - 3000 Mpc"},{"citing_arxiv_id":"2510.02515","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neural Post-Einsteinian Test of General Relativity with the Third Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2025-10-02T19:42:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Neural post-Einsteinian analysis of GWTC-3 finds no GR violation and sets constraints covering both post-Newtonian and beyond-post-Newtonian deviations in a single theory-agnostic setup.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.08099","ref_index":195,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black Hole Spectroscopy and Tests of General Relativity with GW250114","primary_cat":"gr-qc","submitted_at":"2025-09-09T19:17:32+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GW250114 data confirm the remnant is consistent with a Kerr black hole and bound the dominant quadrupolar mode frequency to within a few percent of the GR prediction, with constraints tighter than prior multi-event catalogs.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Speagle, dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evidences, Mon. Not. Roy. Astron. Soc.493, 3132 (2020), arXiv:1904.02180 [astro- ph.IM]. [194] D. M. Macleod, J. S. Areeda, S. B. Coughlin, T. J. Massinger, and A. L. Urban, GWpy: A Python package for gravitational- wave astrophysics, SoftwareX13, 100657 (2021). [195] D. Macleod, S. Coughlin, A. Southgate, D. Davis, M. Pitkin, J. Areeda, R. N. George, P. Altin, P. Godwin, L. Singer,et al., gwpy/gwpy: Gwpy 3.0.9 (2024). [196] A. Collette,Python and HDF5(O'Reilly, 2013). [197] F. Perez and B. E. Granger, Ipython: A system for interactive scientific computing, Computing in Science & Engineering9, 21 (2007). [198] T."},{"citing_arxiv_id":"2509.08054","ref_index":172,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GW250114: testing Hawking's area law and the Kerr nature of black holes","primary_cat":"gr-qc","submitted_at":"2025-09-09T18:00:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GW250114 data confirm the remnant black hole ringdown frequencies lie within 30% of Kerr predictions and that the final horizon area is larger than the sum of the progenitors' areas to high credibility.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Brito, A. Buonanno, and V . Raymond, Black-hole Spec- troscopy by Making Full Use of Gravitational-Wave Model- ing, Phys. Rev. D98, 084038 (2018), arXiv:1805.00293 [gr- qc]. [171] R. Abbottet al.(LIGO Scientific, Virgo), GW190521: A Bi- nary Black Hole Merger with a Total Mass of 150M ⊙, Phys. Rev. Lett.125, 101102 (2020), arXiv:2009.01075 [gr-qc]. 23 [172] R. Abbottet al.(LIGO Scientific, Virgo), Properties and As- trophysical Implications of the 150 M ⊙ Binary Black Hole Merger GW190521, Astrophys. J. Lett.900, L13 (2020), arXiv:2009.01190 [astro-ph.HE]. [173] C. D. Capano, M. Cabero, J. Westerweck, J. Abedi, S. Kastha, A. H. Nitz, Y .-F. Wang, A. B. Nielsen, and B. Krishnan, Mul- timode Quasinormal Spectrum from a Perturbed Black Hole,"},{"citing_arxiv_id":"2507.08219","ref_index":143,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\\odot}$","primary_cat":"astro-ph.HE","submitted_at":"2025-07-10T23:52:46+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":9.0,"formal_verification":"none","one_line_summary":"A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"in the high-spin regime, eccentricity, GW memory, or noise artefacts) one might therefore expect the models to in- teract with these features differently and display model systematics, as are seen in the posteriors for this event. The accuracy of these models for typical signals has been comprehensively assessed through comparison to NR, both in the modelling papers themselves and elsewhere (Mac Uilliam et al. 2024, e.g., [).For GW231123 we have performed the accuracy analysis in Section 4.2, and a series of targeted NR injections, which we now describe. We hope that more can be learned in the future from improved models in the high-spin regime, and a detailed study of the behaviour of our models in Gaussian noise. In order to investigate the likelihood of the presence of waveform systematics in the high total mass, comparable- mass (q >1/3), highly precessing region of parameter space, we perform a simulation study where we simulate a set of signals consisting of highly precessing NR waveforms from the SXS catalog (Boyle et al. 2019; Scheel et al. 2025) and recover with the five waveform models under consideration. From several tens of simulations, we discuss here the results from two that span the range of observed results, from unbiased parameter estimation displaying no systematics to large systematic differences between models and clear biases in parameter recovery. For both configurations, we show the total mass and mass ratio as measured in the data (the detector frame). For high-mass binaries, we expect the total mass to be one of the most reliably measured quantities. The detector-frame masses are not the true source masses, but theredshiftedmasses, and to calculate the true masses, we must also measure the redshift. The relative accuracy of the detector-frame and source-frame masses may therefore differ, depending on 28 Figure 8.Marginalized posterior probability for (left column) redshifted (detector-frame) total binary mass and the mass ratio a"},{"citing_arxiv_id":"2505.08089","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Assessment of normalizing flows for parameter estimation on time-frequency representations of gravitational-wave data","primary_cat":"gr-qc","submitted_at":"2025-05-12T21:49:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GP15 maps BBH spectrograms to parameter posteriors via residual networks and normalizing flows, producing results consistent with LVK analyses on GWTC-2.1 and GWTC-3 events while running in seconds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2406.03568","ref_index":104,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with GW230529: a neutron star merging with a lower mass-gap compact object","primary_cat":"gr-qc","submitted_at":"2024-06-05T18:30:33+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Parameterized inspiral tests on GW230529 find consistency with GR, with |δφ̂_{-2}| ≲ 8×10^{-5} and ℓ_GB ≲ 0.51 M_⊙ in ESGB theories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.14286","ref_index":158,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA","primary_cat":"gr-qc","submitted_at":"2024-04-22T15:37:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bayesian inference on LVK O1-O3 events with eccentric aligned-spin waveforms yields log10 Bayes factors of 1.77-4.75 favoring eccentricity for GW200129, GW190701 and GW200208_22, and >99.5% probability that at least one of 57 events is eccentric under an astrophysically motivated rate prior.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"This can then be propagated into Eqs. (2.10) and (2.11). C. DINGO We now summarize the main features of the machine- learning code DINGO [152-154]. In particular, its use of normalizing flows[155, 156] and importance sampling [115, 157]. In many practical applications, obtainingp(ϑϑϑ|d) in Eq. (2.1) is analytically impossible. But one can use techniques such as nested sampling [158] or Markov-Chain Monte-Carlo (MCMC) [159] to sample from p(ϑϑϑ|d). The LVK Collab- oration has developed tools such as LALInference [160] and Bilby [161-163] for this task. However, these methods must evaluate the likelihood O(107−8) times per event. Thus, for time-domain waveform models produced by solving or- dinary differential equations parameter estimation can be ex-"},{"citing_arxiv_id":"2111.03606","ref_index":159,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2021-11-05T16:43:17+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GWTC-3 catalogs 90 compact binary coalescence events with p_astro > 0.5 from LIGO and Virgo's first three observing runs, including the first confident neutron star-black hole binaries.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Becaue of the correlations between masses and spins [152-154], multimodality in mass distributions may also translate to multiple peaks in the effective inspiral spin distribu- tion. Multimodality can arise due to the complexity of the likelihood surface when using waveform models that include higher-order multipole moments [19, 155- 157] and precession [158, 159], noise fluctuations for quiet signals [160], the presence of glitches [161-163], or there being multiple overlapping signals in the data (which is unlikely given O3 sensitivity) [164]. Therefore, multi- modality is expected in a few cases. Cases with significant multimodality are GW200208 222617, GW200308 173609 and GW200322 091133. These candidates have modest"},{"citing_arxiv_id":"2108.01045","ref_index":298,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_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","primary_cat":"gr-qc","submitted_at":"2021-08-02T17:09:29+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GWTC-2.1 adds eight new high-significance compact binary coalescence events to the prior catalog, extending the observed black hole mass range and including candidates inside the pair-instability mass gap.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"timation was performed with the Bilby library [140, 165] using the Dynesty nested sampling package [297], the RIFT library [171-173] and the LALInference li- brary [137]. PESummary was used to post-process and collate parameter-estimation results [174]. The various 30 stages of the parameter-estimation analysis were man- aged with the Asimov library [298]. Plots were prepared with Matplotlib [299], seaborn [300] and GWpy [87]. NumPy [301] and SciPy [302] were used in the prepara- tion of the manuscript. Appendix A: Estimation of source parameters 1. Binary black holes from the first and second observing runs In order to provide a self-consistent set of source prop- erties, inferred using the state-of-the-art BBH waveform"},{"citing_arxiv_id":"2010.14527","ref_index":233,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2020-10-27T18:01:31+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"GstLAL-based inspiral software pipeline [110, 121, 122] built on the LALSuite software library [287], and with the PyCBC [29, 123-126] and cWB [111, 117- 120] packages. Parameter estimation was performed with the LALInference [177] and LALSimulation libraries within LALSuite [287], the Bilby and Parallel Bilby libraries [230-232] using the dynesty nested sampling package [233], and the RIFT library [227-229]. PESum- mary was used to post-process and collate parameter es- timation results [235]. Estimates of the noise spectra and glitch models were obtained using BayesWave [106, 107, 180]. The cWB and BayesWave packages were also used to generate waveform reconstructions. Plots were prepared with Matplotlib [288], Seaborn [289] and"},{"citing_arxiv_id":"2006.00714","ref_index":262,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian inference for compact binary coalescences with BILBY: Validation and application to the first LIGO--Virgo gravitational-wave transient catalogue","primary_cat":"astro-ph.IM","submitted_at":"2020-06-01T04:46:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"BILBY is validated on simulated compact binary signals and reproduces the eleven GWTC-1 results with configuration and output files provided for reproduction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.02970","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Beyond UVJ: More Efficient Selection of Quiescent Galaxies With UV / Mid-IR Fluxes","primary_cat":"astro-ph.GA","submitted_at":"2019-07-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"UVJ colors saturate below log(sSFR) ~ -10.5; new UV/MIR color-color diagrams allow more efficient selection of galaxies with substantially lower ongoing star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}