{"total":25,"items":[{"citing_arxiv_id":"2605.12606","ref_index":2,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Radio sirens: inferring $H_0$ with binary black holes and neutral hydrogen in the era of the Einstein Telescope and the SKA Observatory","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T18:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Using simulated binary black hole mergers and neutral hydrogen maps, the radio sirens method constrains H0 to 8% precision with 3000 high-SNR events, offering a 90% improvement over standard dark siren analyses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11283","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black Hole Binary Detection Landscape for the Laser Interferometer Lunar Antenna (LILA): Signal-to-Noise Calculations & Science Cases","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T22:09:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Here, we set the angular frequency to beΩ =πfr, wheref r is the rest-frame GW frequency, which is twice the orbital frequency. The root-mean-square of the GW strain, averaging over polarization modes, time (one wave period), and inclination (assuming isotropy) is: h(f) =⟨h 2 ++h2 ×⟩1/2 ι,t = Ω 2π Z π/Ω 0 dt Z 1 −1 d(cosι) [h2 + +h 2 ×] !1/2 = r 2 5 h0 = 8π2/3 √ 10 (GMc)5/3 D(z)c 4 [f(1+z)] 2/3 (2) where the observed frequencyfis related to the rest-frame frequencyfr byf=f r(1 +z) −1. Based on the average strain above, the characteristic strain of an orbiting and inspiraling black hole binary over an observation period oftobs can be modeled by the following piecewise function (Sesana et al., 2005): hc(f)≈    h(f) √f tobs ∝f 7/6 ifn > f t obs"},{"citing_arxiv_id":"2605.11193","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Prospects for multi-messenger discovery of the gravitational-wave background anisotropies via cross-correlation with galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T19:58:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"New simulations show that cross-correlating gravitational wave background anisotropies with galaxy distributions can enable discovery at angular scales of 4-6 degrees with next-generation observatories.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"3.2 Multi-messenger cross-correlation of the SGWB with the galaxy distribution Similarlytotheautocorrelation,thecross-correlationestimatortakes themeanvalueofthesphericallydecomposedcoefficientsofthetwo tracers, namely the SGWB (𝛿ˆΩℓ,𝑚) and the galaxy field (ˆΔℓ′ ,𝑚′): ˆ𝐶GW,g ℓ =⟨𝛿 ˆΩℓ,𝑚 ˆΔℓ′ ,𝑚′ ⟩| ℓ=ℓ ′ ,𝑚=𝑚 ′ = 1 2ℓ+1 ℓ∑︁ 𝑚=−ℓ 𝛿 ˆΩℓ,𝑚 ˆΔ∗ ℓ,𝑚 . (13) The noise coefficients are not independent, since CBCs occur insidegalaxies.Thisgivesrisetoacross-correlationshotnoiseterm 𝑆GW,g: ⟨𝑠GW ℓ,𝑚 𝑠g∗ ℓ,𝑚 ⟩≠⟨𝑠 GW ℓ,𝑚 ⟩⟨𝑠 g ℓ,𝑚 ⟩=⇒ ⟨ ˆ𝐶GW,g ℓ ⟩=𝐶 GW,g ℓ +𝑆 GW,g .(14) WhiletheanalogoustermintheSGWBautocorrelationwasshown tobesubdominant,itbecomesparticularlyrelevanthere,asitgener- ates a shot noise bias that cannot be avoided."},{"citing_arxiv_id":"2605.09250","ref_index":25,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework","primary_cat":"gr-qc","submitted_at":"2026-05-10T01:28:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A unified confluent HeunC framework computes gravitational-wave fluxes from generic Kerr orbits with 10^{-11} relative errors and speedups of 3-60x over existing packages for low- and high-order modes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05563","ref_index":1,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"How do the LIGO-Virgo-KAGRA's Heavy Black Holes Form? No evidence for core-collapse Intermediate-mass black holes in GWTC-4","primary_cat":"astro-ph.HE","submitted_at":"2026-05-07T01:12:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No evidence for core-collapse formed low-spin IMBHs in GWTC-4, with 90% upper limit on merger rate of 0.077 Gpc^{-3} yr^{-1}, low-spin BH mass truncation at 65 solar masses consistent with pair-instability gap lower edge, and high-spin IMBHs from hierarchical mergers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04896","ref_index":100,"ref_count":1,"confidence":0.98,"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":"2605.02882","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tracing Primordial Gravitational Waves via non-Gaussian Signatures of Halo Bias","primary_cat":"astro-ph.CO","submitted_at":"2026-05-04T17:51:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Tensor-induced non-Gaussianity from primordial gravitational waves generates a unique scale-dependent halo bias correction that can reach order-one amplitude for rare high-redshift halos at z=7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02820","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational-Bumblebee perturbations: Exact decoupling and isospectrality","primary_cat":"gr-qc","submitted_at":"2026-05-04T16:57:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bumblebee gravity perturbations decouple exactly into gravitational and vector sectors, with gravitational modes dynamically immune to Lorentz violation and odd-even parities strictly isospectral.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02633","ref_index":71,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Axial tidal Love numbers of black holes in matter environments","primary_cat":"gr-qc","submitted_at":"2026-05-04T14:20:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Axial tidal Love numbers for black holes in anisotropic fluid environments are derived analytically and numerically, with non-compact support density profiles producing logarithmic terms that obstruct standard tidal matching due to the lack of a strictly vacuum exterior.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01992","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reviving Motivated Inflationary Potentials with $K$-inflation in the light of ACT","primary_cat":"gr-qc","submitted_at":"2026-05-03T17:48:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"K-inflation with non-canonical kinetic term G(φ) shifts α-attractor T-models and natural inflation into the Planck-ACT-LB-BK18 allowed region while satisfying Swampland conjectures and producing testable GW spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25916","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nonlocal-in-time tail effects in gravitational scattering to fifth Post-Minkowskian and tenth self-force orders","primary_cat":"hep-th","submitted_at":"2026-04-28T17:59:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Nonlocal-in-time conservative tail contributions to gravitational scattering are derived at 5PM and 10SF orders, expressed via polylogarithms up to weight three and agreeing with prior results through 6PN.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25536","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Large-Eccentricity Asymptotics and Fast Analytic Approximation for Fourier modes of Post-Newtonian Eccentric Waveforms","primary_cat":"gr-qc","submitted_at":"2026-04-28T12:04:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Derives large-eccentricity asymptotics for post-Newtonian eccentric waveform Fourier modes and builds a fast endpoint-constrained analytic approximation with error under 10^{-3} valid to p=200.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24433","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Geometry of transient gravitational waves and estimation of efficiencies of different detector configurations","primary_cat":"gr-qc","submitted_at":"2026-04-27T13:01:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A geometrical method is introduced for analyzing transient gravitational waves to estimate efficiencies of different detector configurations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.22462","ref_index":200,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Machine Learning for Multi-messenger Probes of New Physics and Cosmology: A Review and Perspective","primary_cat":"hep-ph","submitted_at":"2026-04-24T11:29:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A review summarizing machine learning methods for multi-messenger probes of dark matter and new physics, with a proposed plan for future integrated analyses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Concerning applications inspired by collider physics, we identify the following points of immediate relevance for data analysis and dark-matter phenomenology: 1. Reliable models have been developed to simulate nuclear interactions in contexts such as ion therapy, including the Boltzmann-Langevin One Body (BLOB) model or efforts in QCD matter at extreme conditions [200], which describes heavy-ion interactions up to a few hundreds of MeV [211]. In this approach, the final state is represented as a probability density function (PDF) describing the likelihood of finding a nucleon at a given point in phase space. Due to the large computational cost of BLOB simulations, deep-learning-based emulation strategies have been developed [193]."},{"citing_arxiv_id":"2604.18669","ref_index":87,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hawking area law in quantum gravity","primary_cat":"gr-qc","submitted_at":"2026-04-20T17:59:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Exact Hawking area law from black hole mergers restricts quantum gravity to singular Ricci-flat or specific regular black holes in Stelle and nonlocal theories, derives the standard entropy-area law, and realizes Barrow fractal black holes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"possible to place stringent bounds on anything deviating from Einstein gravity, from the mass and speed of the graviton to violations of Lorentz invariance [83-85]. So far, there is no evidence of new physics but the field is in rapid evolution and we have not exhausted all its possi- bilities. Third-generationdetectorssuchasLISA[86]and Einstein Telescope [87] are further expanding the battery of tests and the range of models of interest. Among the aspects touched by GW observations with momentous ramifications both for general relativity and for quantum gravity is Hawking area law for classical black holes [88]. This law (reviewed below) states that the area of the event horizon of a classical black hole"},{"citing_arxiv_id":"2604.14270","ref_index":8,"ref_count":1,"confidence":0.98,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.13208","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Axial Oscillations of Viscous Neutron Stars","primary_cat":"gr-qc","submitted_at":"2026-04-14T18:30:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Viscous neutron stars have new families of axial oscillation modes without perfect-fluid counterparts, featuring mode avoidance and long-lived modes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.11903","ref_index":7,"ref_count":1,"confidence":0.98,"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":"LVK, LISA, and joint observations, Gen. Rel. Grav.54, 133 (2022), arXiv:2207.10096 [gr-qc]. [5] N. Afshordiet al.(LISA Consortium Waveform Work- ing Group), Waveform modelling for the Laser Interfer- ometer Space Antenna, Living Rev. Rel.28, 9 (2025), arXiv:2311.01300 [gr-qc]. [6] A. Abacet al.(ET), The Science of the Einstein Tele- scope, (2025), arXiv:2503.12263 [gr-qc]. [7] J. Aasiet al.(LIGO Scientific), Advanced LIGO, Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr- qc]. [8] F. Acerneseet al.(VIRGO), Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. Quant. Grav.32, 024001 (2015), arXiv:1408.3978 [gr-qc]. [9] T. Akutsuet al.(KAGRA), KAGRA: 2.5 Generation In- terferometric Gravitational Wave Detector, Nature As-"},{"citing_arxiv_id":"2604.11895","ref_index":85,"ref_count":1,"confidence":0.98,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.11871","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Not too close! Evaluating the impact of the baseline on the localization of binary black holes by next-generation gravitational-wave detectors","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Baselines of 8-11 ms light travel time for two CE detectors provide a reasonable compromise for BBH sky localization, with third detectors eliminating multimodality for most or all events.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.08679","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tidal Response of Compact Objects","primary_cat":"gr-qc","submitted_at":"2026-04-09T18:10:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"This review summarizes tidal Love numbers and dissipation effects for black holes, neutron stars, and exotic objects, noting vanishing static bosonic Love numbers for black holes in GR but nonzero values for fermions and exotic objects, with implications for gravitational-wave astronomy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"choices, the options (c) and (d), as described above, does not have a decaying mode, and hence provides vanishing LNs for the axial vector perturbations. While they yield non-zero answers for the other two, namely options (a) and (b). In particular, for option (a), i.e., for non-integer and non-half-integer values of ˆℓ, we have, 1k(non-integer) ℓm(v) = 2ˆℓ + 1 Γ(2ˆℓ + 2)2 ! Γ \u0012 ˆℓ + 1 − 1 d − 3 \u00132 Γ \u0012 ˆℓ + 1 + 1 d − 3 \u00132 × sin[π(ˆℓ − 1 d−3)] sin[π(ˆℓ + 1 d−3)] π sin \u0010 2πˆℓ \u0011 . (3.64) 78 Finally, for half-integer values of ˆ ... [truncated to fit review budget] ..."},{"citing_arxiv_id":"2604.08471","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pyramid Interferometers: Direct Access to Cosmological Gravitational Wave Chirality","primary_cat":"gr-qc","submitted_at":"2026-04-09T17:10:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Pyramid interferometers use non-coplanar geometry to create a channel sensitive only to net helicity in the cosmological gravitational wave background while remaining blind to the unpolarized component.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.07302","ref_index":9,"ref_count":1,"confidence":0.98,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.06312","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black Hole-Boson Star Binaries: Gravitational Wave Signals and Tidal Disruption","primary_cat":"gr-qc","submitted_at":"2026-04-07T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical simulations of black hole-boson star binaries show that scalar self-interactions can suppress tidal disruption while radiative efficiency depends on the chosen potential.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.06009","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Are Black Holes Fuzzballs? Probing Horizon-Scale Structure with LISA","primary_cat":"hep-th","submitted_at":"2026-04-07T16:05:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}