{"total":34,"items":[{"citing_arxiv_id":"2606.30144","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Joint population and strong-lensing inference for resolved gravitational-wave events probes the black-hole merger rate beyond the peak of star formation","primary_cat":"astro-ph.HE","submitted_at":"2026-06-29T11:21:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Joint strong-lensing and population inference on resolved gravitational-wave events finds no lensed events and tightens constraints on the black-hole merger rate peak redshift and high-redshift tail.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21824","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors","primary_cat":"astro-ph.HE","submitted_at":"2026-06-20T01:25:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06209","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The first decade of gravitational-wave measurements of black hole spins","primary_cat":"gr-qc","submitted_at":"2026-06-04T14:14:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"A review summarizing formation-channel predictions, waveform effects, and population-level constraints on stellar-mass black hole spins from the first decade of gravitational-wave observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Keywords:binary black holes; black hole spin; gravitational waves 1. Introduction A decade after the first direct detection of gravitational waves, the catalog of sources detected by the LIGO-Virgo-KAGRA (LVK) collaboration has grown to include hundreds of binary black holes (BBHs) mergers, two binary neutron stars, and a few neutron star-black hole (NSBH) mergers [ 1-3]1. Astrophysical black holes are characterized by only two parameters-their masses and spins-which leave imprints on the gravitational waveform of each compact-object merger event. Thus, analyses of the gravitational-wave ( GW) strain data recorded in interferometric detectors allow us to constrain the parameters characterizing each binary and the population as a whole."},{"citing_arxiv_id":"2605.20112","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational-wave constraints on $H_0$ are robust to (putative) redshift evolution in the binary black hole mass spectrum at current sensitivity","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T16:59:39+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Spectral-siren H0 constraints from GWTC-4.0 binary black holes remain robust when the mass spectrum is permitted to evolve with redshift at current detector sensitivity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19153","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GstLAL O4 Online Results Paper","primary_cat":"gr-qc","submitted_at":"2026-05-18T22:15:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"GstLAL produced low-latency alerts for 250 astrophysically plausible gravitational-wave candidates during O4, providing the first upload for 222 and the sole upload for 75, with 88 percent of significant catalog events detected and 93 percent classification agreement.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18097","ref_index":50,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effects of formation channels and gravitational lensing on stochastic gravitational wave background","primary_cat":"gr-qc","submitted_at":"2026-05-18T09:11:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Using HBI on GWTC-4 data the authors compute lensed SGWBs for ABHs and PBHs and conclude that LIGO and ET can distinguish the two formation channels in specific frequency ranges, with ET offering broader coverage.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16506","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Rapidly Rotating Neutron Star Collapse in Massive Scalar-Tensor Theories","primary_cat":"gr-qc","submitted_at":"2026-05-15T18:01:51+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Numerical simulations of collapsing scalarized neutron stars show scalar radiation energy of order 10^{-3} solar masses, orders of magnitude above the tensor quadrupolar emission, potentially observable to test modified gravity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15749","ref_index":42,"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":"2605.15265","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T18:00:00+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11703","ref_index":5,"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":"advantage of the small statistical uncertainties offered by high SNRs, we must ensure small systematic uncertainties. Fortunately, GW signals can be used to constrain the detec- tor response directly. Thisastrophysicalcalibration approach leverages accurate modeling of GW waveforms, allowing the astrophysical signal to serve as an independent reference for the frequency-dependent detector calibration [5, 25, 26]. As- trophysical calibration may be performed in a variety of ways: using the frequency and amplitude evolution of the (predicted) signal to infer calibration parameters together with source pa- rameters [26-28]; using an electromagnetic counterpart (and assumed cosmology) to establish the distance to a source [29], which provides more information than using the GW signal"},{"citing_arxiv_id":"2605.11274","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"End-to-End Population Inference from Gravitational-Wave Strain using Transformers","primary_cat":"gr-qc","submitted_at":"2026-05-11T21:54:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dingo-Pop uses a transformer to perform amortized, end-to-end population inference from GW strain data in seconds, bypassing per-event Monte Carlo sampling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"of 25 to 1000 events, and obtain well-calibrated posteriors consistent with traditional methods. By avoiding per-event analyses that can take hours to days,Dingo-Popenables new classes of large-scale injection studies; as an application, we examine how spectral-siren Hubble constant uncertainties change with catalog size. Introduction.-Population inference is now central to gravitational-wave (GW) astronomy. The latest catalog, GWTC-4.0 [1, 2], contains 218 events observed by the LIGO-Virgo-KAGRA Collaboration (LVK) [ 3-5]. By combining information across events, one can measure merger rates and source distributions [ 6], perform tests of general relativity [ 7], and constrain the expansion of the universe [ 8]. Current approaches, however, rely on hierarchical Bayesian analysis (HBA) methods built on"},{"citing_arxiv_id":"2605.04896","ref_index":113,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Parameter Estimation Horizon of Core-Collapse Supernovae with Current and Next-Generation Gravitational-Wave Detectors","primary_cat":"astro-ph.HE","submitted_at":"2026-05-06T13:27:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Machine learning extracts core rotation and signal properties from CCSN gravitational waves, with next-generation detectors constraining rotation beyond 100 kpc for favorable orientations despite some uncertainties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23835","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Squeezed state degradations due to mode mismatch and thermal aberrations in gravitational wave detectors","primary_cat":"physics.ins-det","submitted_at":"2026-04-26T18:42:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Thermal aberrations induce low-pass frequency dynamics for quadratic wavefront mismatches and high-pass dynamics for higher-order aberrations, degrading squeezed states differently in current versus future gravitational wave detectors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Ξ(Ω) = [|rrse(+Ω)| − |r∗ rse(−Ω)|]2 4Γ(Ω)η(Ω) .(40) This phase noise can be understood by the fact that the noise in the upper and lower sidebands of a squeezed vacuum is increased relative to that of the unsqueezed vacuum, but in a correlated way so that the noise in one quadrature is reduced while the noise in the orthog- onal quadrature is increased [ 4, 42]. A phase noise is thus introduced when the sidebands experience different losses which preserve the increased noise while degrading the correlations responsible for defining the angle of the squeeze ellipse [ 12]. The phase noise generated by this intrinsic dephasing is shown as the dotted green line in Fig. 4. The other non-green dashed curves in Fig."},{"citing_arxiv_id":"2604.22437","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Spontaneous spherical symmetry breaking of black holes with resonant hair","primary_cat":"gr-qc","submitted_at":"2026-04-24T10:54:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Black holes with resonant hair spontaneously break spherical symmetry and decay into bald black holes via non-spherical dynamics, either through fission or absorption.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.15885","ref_index":18,"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":"ppop(θ|d,{d n})∝ L(d|θ)p pop(θ|{dn}) (3) for the parametersθof a new event with datadcan be informed independently by the existing catalog with the priorp pop(θ|{dn}) = R dλ ppop(θ|λ)ppop(λ|{dn}). We assess the effect on the source properties of GW241011 and GW241110 using the population model above and a second model defined in terms of the effective spin [18, 37] χeff = m1χ1 cosτ 1 +m 2χ2 cosτ 2 m1 +m 2 (4) instead ofχ 1,2 andτ 1,2, described in the End Matter. 4 0 2 4 6 8 10 12 14Probability density GW241110 GW241011 Single event Population informed χi, τi Population informed χeff 0 2 4 6 8 10 12 14Probability density Lowest χeff extremizing with GW241011 GW241110 Highest χeff extremizing with GW241011"},{"citing_arxiv_id":"2604.15759","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Mechanical Long Baseline Differential Gradiometers as Low Frequency Gravitational Wave Detectors","primary_cat":"gr-qc","submitted_at":"2026-04-17T07:01:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A vertical long-wire suspended gradiometer configuration amplifies gravitational wave signals from order h to order h L/D by separating gravitational force from moment of inertia.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.13687","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"VIGILant: an automatic classification pipeline for glitches in the Virgo detector","primary_cat":"gr-qc","submitted_at":"2026-04-15T10:09:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"VIGILant applies tree-based models and a ResNet CNN to classify Virgo O3b glitches with 98% accuracy and has been deployed for daily use with an interactive dashboard.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"monitoring glitches and mitigating their harmful effect is a crucial activity for characterizing the detectors and in- creasing their sensitivity. The efforts to diagnose and mitigate glitches are the responsibility of the Detector Characterization groups in the LVK collaboration [11, 13], with Machine Learning (ML) approaches playing an increasingly important role in these studies [14]. A key investigation involves the classification of glitches into classes, each of which has a distinctive morphology in its time-frequency representa- tion. Grouping glitches into classes is helpful for noise hunting, as one can look for correlations between a class of glitches and the detectors' auxiliary channels, which measure the status of the detector and the environment."},{"citing_arxiv_id":"2604.13580","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Investigating the effect of sensitivity of KAGRA on sky localization of gravitational-wave sources from compact binary coalescences","primary_cat":"gr-qc","submitted_at":"2026-04-15T07:39:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"KAGRA enhances sky localization of binary neutron star mergers in the LVK network via added baselines, with measurable gains at current sensitivity and larger improvements as range reaches ~30 Mpc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.08653","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Love numbers of black holes and compact objects","primary_cat":"gr-qc","submitted_at":"2026-04-09T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"radiation took humanity rather longer to detect than its electromagnetic counterpart. Gravitational wave astronomy has since matured into a full-fledged observational science. The global detector network LIGO- Virgo-KAGRA (LVK) has accumulated a steady stream of events; as of the fourth observing run (O4), the catalog stands at around 300 binary black hole mergers [2-5]. The gravitational-wave sources we observe at present are binary systems of compact objects. Bycompact we mean a body whose massMis confined within a radius comparable to its Schwarzschild radius, rs≡2GM c2 , where G is the Newtonian gravitational constant, so that its gravitational field is within the strong gravity régime where the effects of general relativity are important."},{"citing_arxiv_id":"2604.07302","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravitational wave signal and noise response of an optically levitated sensor in a Fabry-P\\'erot cavity","primary_cat":"gr-qc","submitted_at":"2026-04-08T17:11:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A general relativistic derivation of gravitational wave response in an optically levitated cavity sensor reveals position-dependent strain sensitivity and suppressed input-mirror noise coupling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(LIGO Scientific, KAGRA, VIRGO), GWTC-4.0: An Introduction to Version 4.0 of the Gravitational-Wave Transient Catalog, Astrophys. J. Lett.995, L18 (2025), arXiv:2508.18080 [gr-qc]. [5] G. Agazieet al.(NANOGrav), The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background, Astrophys. J. Lett.951, L8 (2023), arXiv:2306.16213 [astro-ph.HE]. [6] J. Antoniadiset al.(EPTA, InPTA), The second data re- lease from the European Pulsar Timing Array - V. Search for continuous gravitational wave signals, Astron. Astro- phys.690, A118 (2024), arXiv:2306.16226 [astro-ph.HE]. [7] A. Abacet al.(ET), The Science of the Einstein Tele- scope, (2025), arXiv:2503.12263 [gr-qc]. [8] E. D. Hall, Cosmic Explorer: A Next-Generation"},{"citing_arxiv_id":"2604.06090","ref_index":97,"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":"background","top_context_polarity":"unclear","context_text":"We consider catalogs of 70 BBH events (the approxi- mate number of events in GWTC-3.0) and use the same individual-event likelihood models investigated in Miller et al.[36], corresponding to different noise scenarios: 1.Realistic O3 noise likelihood: Individual-event posteriors were sampled stochastically via nested sampling [96] with the parameter-estimation code Bilby[97], using realistic O3 sensitivity [98] and the waveform modelIMRPhenomXPHM[99]. 2.Gaussian likelihood: Individual-event spin mag- nitude and cosine-tilt posteriors were constructed using simulated Gaussian likelihoods with stan- dard deviationsσ meas = 0.1,0.3,0.5. Samples from the Gaussian spin posteriors were randomly paired with those from the full stochastically sampled"},{"citing_arxiv_id":"2604.05492","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Remnant recoil and host environments of GWTC-4.0 binary black-hole mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-04-07T06:34:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Five O4 gravitational-wave events prefer dynamical cluster formation; typical recoil kicks eject remnants from globular clusters but allow possible retention in nuclear star clusters, disfavoring efficient hierarchical growth in globular clusters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"monics,θ, φare the polar and azimuthal angles of the binary in the sky, andh ℓ,m are the waveform modes. For non-precessing binaries with spins aligned or anti- aligned with the orbital angular momentum ˆL, the system is in- variant under reflection across the orbital plane. In a frame where thez-axis is aligned with ˆLthis equatorial symmetry enforces the relation hℓ,m(t)=(−1) ℓ h∗ ℓ,−m(t),(2) Article number, page 2 J. Llobera-Querol et al.: Remnant recoil and host environments of GWTC-4.0 binary black-hole mergers where ∗ denotes complex conjugate. This symmetry enforces ex- act cancellations in the linear-momentum flux perpendicular to the orbital plane. When the component spins are misaligned with ˆL, relativis- tic spin-orbit coupling induces precession and the equatorial"},{"citing_arxiv_id":"2603.06010","ref_index":21,"ref_count":1,"confidence":0.9,"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":"V. Oloworaran, F. Panther, J. Powell, A. S. Sengupta, K. Wette, and X. Zhu, Physical Review D105, 024023 (2022), arXiv:2011.06787 [gr-qc]. [20] S. Klimenko, G. Vedovato, M. Drago, F. Salemi, V. Ti- wari, G. A. Prodi, C. Lazzaro, K. Ackley, S. Tiwari, C. F. da Silva, and G. Mitselmakher, Physical Review D93, 042004 (2016), arXiv:1511.05999 [gr-qc]. [21] M. Drago, V. Gayathri, S. Klimenko, C. Lazzaro, E. Milotti, G. Mitselmakher, V. Necula, B. O'Brian, G. A. Prodi, F. Salemi, M. Szczepanczyk, S. Tiwari, V. Tiwari, G. Vedovato, and I. Yakushin, SoftwareX14, 100678 (2021), arXiv:2006.12604 [gr-qc]. [22] F. Robinet, N. Arnaud, N. Leroy, D. Macleod, and J. McIver, SoftwareX12, 100620 (2020), arXiv:2007."},{"citing_arxiv_id":"2602.11282","ref_index":127,"ref_count":1,"confidence":0.9,"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":"background","top_context_polarity":"background","context_text":"The sequence of steps can be understood reading Eq. (B1) right to left. We follow the procedures in Refs. [73, 84] to perform these simulations. In summary: GW signals are gener- ated using theIMRPhenomXPwaveform model [126]; Gaussian noise for the LIGO Hanford, LIGO Livingston, and Virgo detectors is generated according to their O4 design power spectral densities [127, 128]; data contain- ing signal and noise is classed as detected if the matched- filter signal-to-noise ratio (SNR) [129] is greater than 11 [130, 131] (note that this is technically an unphys- ical selection criterion [132] as the matched-filter SNR is computed using the true signal parameters, which in reality are not directly accessible from the data, and"},{"citing_arxiv_id":"2601.18835","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Beyond FINDCHIRP: Breaking the memory wall and optimal FFTs for Gravitational-Wave Matched-Filter Searches with Ratio-Filter Dechirping","primary_cat":"astro-ph.IM","submitted_at":"2026-01-25T20:45:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Ratio-Filter Dechirping converts gravitational-wave matched filtering from a memory-bound FFT into a cache-efficient FIR convolution, delivering a measured 8x speedup in the core loop.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.10806","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Shadow signatures and energy accumulation in Lorentzian-Euclidean black holes","primary_cat":"gr-qc","submitted_at":"2026-01-15T19:15:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Lorentzian-Euclidean black holes produce excess inner-shadow intensity and accumulate energy at the horizon with backreaction unlike stable light rings.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.09678","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The impact of waveform systematics and Gaussian noise on the interpretation of GW231123","primary_cat":"gr-qc","submitted_at":"2026-01-14T18:22:32+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The high mass and high spin magnitudes inferred for GW231123 using NRSur7dq4 are robust to waveform systematics and Gaussian noise.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.21370","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detection of Lensed Gravitational Waves in the Millihertz Band Using Frequency-Domain Lensing Feature Extraction Network","primary_cat":"astro-ph.IM","submitted_at":"2025-12-24T03:58:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"DCL-xLSTM neural network detects lensed GW events with AUC over 0.99 using training on PM and SIS lens models in the millihertz band.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.01387","ref_index":75,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Similar Fermi-GBM sGRBs to GW/sGRB 170817A in MeV-GeV energies","primary_cat":"astro-ph.HE","submitted_at":"2025-12-01T08:02:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Identifies eight Fermi-GBM sGRBs similar to 170817A via hardness-ratio K-means clustering and estimates ~5 GW+sGRB events by end of O4.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.02515","ref_index":17,"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":"2509.14924","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Residual Test for the Third Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2025-09-18T13:00:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Residuals after subtracting best-fit waveforms from GWTC-3 events show no significant deviation from noise according to three standard goodness-of-fit tests.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.08099","ref_index":33,"ref_count":1,"confidence":0.9,"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":"background","top_context_polarity":"background","context_text":"Abacet al.(LIGO Scientific, VIRGO, KA- GRA), GWTC-4.0: An Introduction to Version 4.0 15 of the Gravitational-Wave Transient Catalog, (2025), arXiv:2508.18080 [gr-qc]. [32] GWTC-4.0: Updating the Gravitational-Wave Transient Cata- log with Observations from the First Part of the Fourth LIGO- Virgo-KAGRA Observing Run, (2025), arXiv:2508.18082 [gr-qc]. [33] L. Blanchet and B. S. Sathyaprakash, Detecting a Tail Effect in Gravitational-Wave Experiments, Physical Review Letters 74, 1067 (1995). [34] B. P. Abbottet al.(LIGO Scientific Collaboration, Virgo Col- laboration), Observation of Gravitational Waves from a Bi- nary Black Hole Merger, Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [35] B."},{"citing_arxiv_id":"2509.03360","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Early Career Workshop of GR-Amaldi 2025","primary_cat":"physics.soc-ph","submitted_at":"2025-08-30T17:29:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"The paper reports on the aims, activities, and conclusions of an early-career workshop focused on scientific overviews, transferable skills, and networking in gravitational physics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.21125","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"PRECESSION 2.1: black-hole binary spin precession on eccentric orbits","primary_cat":"gr-qc","submitted_at":"2025-08-28T18:00:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Version 2.1 of the precession code extends post-Newtonian modeling of spinning black-hole binaries to eccentric orbits via a decorator-based adaptation and new evolutionary equations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}