{"total":38,"items":[{"citing_arxiv_id":"2607.08445","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Signal-to-Noise Ratio Contours for LISA","primary_cat":"gr-qc","submitted_at":"2026-07-09T13:08:02+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LISA auto-correlation SNR equals the square root of T_obs times the integral of (signal/(noise+signal))^2 and is therefore bounded by sqrt(T_obs(f_max-f_min)).","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.06154","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pulsars in Globular Clusters With the SKAO","primary_cat":"astro-ph.HE","submitted_at":"2026-07-07T11:32:25+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SKA-MID and SKA-LOW are predicted to discover 150–1700 new pulsars in Galactic globular clusters, more than doubling the current population of 345.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.05331","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling Uncertainties in Modified Gravity Predictions for the Stochastic Gravitational-Wave Background","primary_cat":"astro-ph.CO","submitted_at":"2026-07-06T17:07:48+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Third-generation gravitational-wave detectors can constrain frequency-dependent beyond-GR waveform modifications in the stochastic background, but modified propagation effects remain degenerate with astrophysical population parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31434","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveiling the properties of galaxy cores excavated by supermassive black hole binaries with SHARP","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T10:03:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Next-generation IFU instruments could detect core scouring and tangential anisotropy from MBH binaries up to z~0.14 for ~150 pc cores and higher redshifts for larger cores, expanding searchable volume by 30-40 times including lower-mass systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28937","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quadrupole and quadratic-in-spin effects in quasicircular, spinning, asymmetric binaries","primary_cat":"gr-qc","submitted_at":"2026-06-27T14:17:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Calculates energy fluxes with quadratic-in-spin and quadrupole effects for small-mass-ratio spinning binaries in self-force theory, providing numerical data and sixth-order PN expansions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Holes Due to Inaccurate Gravitational-Wave Models, Phys. Rev. X15, 031036 (2025), arXiv:2404.05811 [gr- qc]. [17] R. S. Chandramouli, K. Prokup, E. Berti, and N. Yunes, Systematic biases due to waveform mismodeling in parametrized post-Einsteinian tests of general relativ- ity: The impact of neglecting spin precession and higher modes, Phys. Rev. D111, 044026 (2025), arXiv:2410.06254 [gr-qc]. [18] P. Mahapatra, J. E. Thompson, E. Fauchon-Jones, and M. Hannam, The High-Mass-Ratio Challenge in Gravi- tationalWaveformModelling, (2026),arXiv:2603.26521 [gr-qc]. [19] S. Marsat, Cubic order spin effects in the dynam- ics and gravitational wave energy flux of compact ob- ject binaries, Class. Quant. Grav.32, 085008 (2015), 30 arXiv:1411.4118 [gr-qc]."},{"citing_arxiv_id":"2606.28512","ref_index":174,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dual AGN and Multiple SMBH Systems in the Era of SKAO","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T18:08:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review outlining radio methods for dual AGN and SMBHB detection and the role of SKAO in enabling comprehensive studies across cosmic time.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27526","ref_index":80,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dynamics of Relativistic Binaries in Structured and Stochastic Environments: A Lagrange-Fourier-Hansen Framework","primary_cat":"gr-qc","submitted_at":"2026-06-25T20:19:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A new framework projects perturbations onto resonant frequencies via Hansen coefficients to produce efficient coupled ODEs for orbital elements in GW-driven relativistic binaries, demonstrated on tidal fields and accretion disks.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"provide a brief discussion of several notable applications. Tidal perturbations, which motivated our first worked example, arise whenever a compact binary evolves in the vicinity of a third massive body. Previous work has shown that such companions can imprint observable signatures on gravitational-wave signals through line- of-sight accelerations [80, 136-139], secular tidal fields [94, 116, 140-142], and even Kozai-Lidov oscillations [92, 143-146]. Beyond these orbit-averaged effects, the motion of the third body introduces explicitly time- dependent forcing through both the eccentric motion of the inner binary and harmonics of the outer orbital fre- quency, which can produce localized resonances."},{"citing_arxiv_id":"2606.25773","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Temporal Correlation Statistic for Intrinsic Phase Fluctuation in Double White Dwarf Gravitational-Wave Signals","primary_cat":"gr-qc","submitted_at":"2026-06-24T12:47:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Introduces a minimal quadratic statistic to isolate temporal correlations in intrinsic phase fluctuations of double white dwarf binaries and derives an analytic SNR scaling with total observation time and intrinsic correlation time.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24070","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nanohertz gravitational waves from domain walls nucleated during inflation","primary_cat":"gr-qc","submitted_at":"2026-06-23T02:28:01+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":"2606.23846","ref_index":178,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial Black Holes: A Review of Formation and Evolution","primary_cat":"gr-qc","submitted_at":"2026-06-22T18:29:10+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"mation and distribution of PBHs, recent advancements have highlighted their potential as unique probes of the high-curvature regime through indirect observational sig- natures. A promising avenue involves the interaction of asteroid-mass PBHs with interstellar media, specifi- cally within the neutral hydrogen (HI) clouds ubiquitous throughout the galaxy. As demonstrated recently [178], the intense local gravitational curvature of a sub-lunar PBH acts as a microscopic tidal perturbator, inducing a quantum-mechanical splitting of the bound internal en- ergy levels of neutral hydrogen atoms. This perturba- tion fundamentally alters the standard 9.9 GHz absorp- tion profile of interstellar hydrogen, redistributing the 28 single spectral line into a distinct, high-bandwidth clus-"},{"citing_arxiv_id":"2606.19995","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Finite-Core Signatures in LISA-Band Wave-Optics Lensing by Low-Mass Dark Matter Halos","primary_cat":"astro-ph.CO","submitted_at":"2026-06-18T09:32:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Finite cores in low-mass dark matter halos produce distinct complex residuals in LISA-band wave-optics amplification that cannot be fully mimicked by lower-concentration NFW profiles and peak at rc/rs ≃ 0.25-0.3.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18341","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Orbital evolution of asymmetric binaries within accreting environments","primary_cat":"gr-qc","submitted_at":"2026-06-16T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Disk-induced dissipation drives rapid orbital plane alignment followed by slower eccentricity damping in extreme mass-ratio inspirals, with relativistic effects producing accumulating deviations from Keplerian orbits even at large separations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11728","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Periodic orbits as probes of charged loop quantum gravity black holes through gravitational waves","primary_cat":"gr-qc","submitted_at":"2026-06-10T07:06:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Periodic orbits in charged LQG black holes produce zoom-whirl gravitational waveforms detectable by future space-based observatories, with features depending on the fixed polymerization parameter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01580","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial black holes spin from cosmological first-order phase transitions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-01T02:26:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The paper derives a quantitative relationship showing that the Kerr parameter a_* of PBHs from first-order phase transitions increases with latent heat α and decreases with transition rate β, reaching typical values of 10^{-3}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01236","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Improving the resolution of double white dwarf systems with spaceborne gravitational wave observatories using a robust astrophysical prior","primary_cat":"gr-qc","submitted_at":"2026-05-31T13:36:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Adding a prior linking GW frequency f to its derivative ḏ from detached white dwarf mass limits to the GBSIEVER iterative pipeline raises resolved DWD sources by ~7.3% for LISA and ~14.6% for the LISA-Taiji network on simulated data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16506","ref_index":11,"ref_count":1,"confidence":0.9,"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":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In massive scalar-tensor gravity, rotating neutron stars that collapse emit nearly the same tensor gravitational waves as in general relativity, but lose about 10^-3 solar masses of energy in scalar radiation - far more than the quadrupole channel.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15265","ref_index":12,"ref_count":2,"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":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations of dynamical channels predict ~36 eccentric stellar-mass BBHs detectable by LISA in the Milky Way at SNR>1 over 10 years, a local merger rate of ~9 Gpc^{-3} yr^{-1}, and hundreds of faint extragalactic mHz sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13847","ref_index":7,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Analytical Fluxes from Generic Schwarzschild Geodesics","primary_cat":"gr-qc","submitted_at":"2026-05-13T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"An analytic Chebyshev-expansion method computes gravitational-wave fluxes from arbitrary-eccentricity Schwarzschild geodesics by reducing them to sums of prior Keplerian Fourier coefficients, with numerical tests showing 10^{-5} total flux accuracy and sub-10^{-6} mode errors for selected cases.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(LISA) [4-6], will enable the first observations of extreme mass-ratio inspirals (EMRIs), events in which a stellar mass compact object inspirals into a much more massive black hole, with typical mass ratios on the range 10 −4 − 10−6. Unlike the short inspiral phase in most mergers observed by ground-based detectors, the inspiral phase of EMRIs can be on the order of years [7]. Maintaining accuracy of gravitational wave templates over such long timescales represents a significant model- ing challenge, and is predominantly tackled using the self- force approach (see, e.g., [8, 9] and references therein). The self-force approach uses the small mass-ratio to de- scribe the phase evolution of EMRI waveforms using a post-adiabatic (PA) expansion, with complete models re-"},{"citing_arxiv_id":"2605.13738","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Inpainting over the cracks: challenges of applying pre-merger searches for massive black hole binaries to realistic LISA datasets","primary_cat":"astro-ph.IM","submitted_at":"2026-05-13T16:15:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Inpainting allows recovery of pre-merger massive black hole binary signals in LISA data despite gaps and overlaps.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"window, and show how removing signals that have been confidently identified from the data allows us to identify quieter signals in the same period. I. INTRODUCTION The Laser Interferometer Space Antenna (LISA) gravitational-wave observatory, planned for launch in the mid-to-late 2030s [1, 2], will unlock our ability to ob- serve the universe in the low-frequency gravitational- wave band [3]. A key science target for LISA is the observation of Massive Black Hole Binaries (MBHBs). These signals are expected to have a very large signal- to-noise ratio, making the problem of identifying them trivial [3]. A significant challenge lies in reliably inferring the parameters of these sources, especially given a large population of other sources present in the data, and this"},{"citing_arxiv_id":"2605.09250","ref_index":23,"ref_count":3,"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 HeunC framework computes gravitational-wave fluxes from generic Kerr orbits with 10^{-11} relative errors and speedups of 3-60x over prior packages by eliminating auxiliary parameters via analytic continuation and adaptive quadrature.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cutler, LISA capture sources: Approxi- mate waveforms, signal-to-noise ratios, and parameter esti- mation accuracy, Phys. Rev. D69, 082005 (2004), arXiv:gr- qc/0310125. [22] J. R. Gair, M. Vallisneri, S. L. Larson, and J. G. Baker, Testing general relativity with low-frequency, space-based gravitational-wave detectors, Living Rev. Rel.16, 7 (2013), arXiv:1212.5575 [gr-qc]. [23] A. Maselli, N. Franchini, L. Gualtieri, T. P. Sotiriou, S. Barsanti, and P. Pani, Detecting fundamental fields with LISA observations of gravitational waves from ex- treme mass-ratio inspirals, Nature Astron.6, 464 (2022), arXiv:2106.11325 [gr-qc]. [24] L. Speri, S. Barsanti, A. Maselli, T. P. Sotiriou, N. Warbur- ton, M. van de Meent, A. J. K. Chua, O."},{"citing_arxiv_id":"2604.26011","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Parameter-estimation bias induced by transient orbital resonances in extreme-mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-04-28T18:00:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":5.0,"formal_verification":"none","one_line_summary":"For most studied EMRI orbits, omitting 3:2, 2:1, 4:3, or 3:1 resonance crossings causes significant SNR loss and Fisher biases exceeding 1σ, with coefficient signs and amplitudes controlling the effect.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"These detectors will be sensitive to new astro- physical sources and augment the information we have so far from ground-based observations. One of the most promising targets is the class represented byextreme- mass-ratio inspirals(EMRIs), in which a stellar-mass compact object of massµspirals into a supermassive black hole (BH) of massM, with mass-ratioη≡µ/M≲ 10−4 [2]. Because of their slow, adiabatic evolution, EMRIs are expected to complete around104-105 orbital cycles prior to merger [3-5], allowing them to potentially stay in LISA's sensitivity band for its entire mission dura- tion. Estimates indicate that LISA could detect up to 103 EMRI events over its nominal4.5-year mission life- time [1, 6, 7]. The GW signal produced by the slow"},{"citing_arxiv_id":"2604.24330","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Pre-localization of Massive Black Hole Binaries in the Millihertz Band","primary_cat":"gr-qc","submitted_at":"2026-04-27T11:21:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A neural spline flow pipeline performs amortized inference on millihertz MBHB signals, delivering ~20 deg² pre-merger sky localizations in ~1 minute while matching PTMCMC sky modes and parameter uncertainties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"TABLE VII. Illustrative tiling times for a 90% credible sky areaA 90 = 20 deg2 with 8 modes Facility FoV [deg 2]t read [s]t exp [s]N tile Imaging time [min] Reference Rubin/LSST 9.6 2 30 8≈8×(30 + 2)/60≈4.3 [69] ZTF 47 10 30 8≈8×(30 + 10)/60≈5.3 [70] Pan-STARRS1 7.068 - 45 - 60 8≈8×60/60 = 8 [71, 72] Athena 0.44 - 10 4 −10 5 46≈46×(10 5)/60 = 76.7 [5, 73] TABLE VIII. Sky localization for 10 independent noise re- alizations of the same injected signal. For each realization, we report the recovered 90% credible sky areaA 90. Since the number of predicted sky modes is consistently 8 across all noise realizations, the number of disconnected sky modes Ntile and the corresponding estimated follow-up time budget"},{"citing_arxiv_id":"2604.20966","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Light, heavy, primordial: exploring the diversity of black hole seeding and growth mechanisms in the JWST era","primary_cat":"astro-ph.GA","submitted_at":"2026-04-22T18:00:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Primordial black holes and heavy astrophysical seeds with super-Eddington accretion reproduce JWST-observed black hole masses, stellar masses, and low metallicities at z~7-10, while light seeds with Eddington-limited accretion are ruled out; PBHs uniquely show a decreasing black hole-to-stellar mass","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19197","ref_index":10,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"CP-violating multi-field phase transitions and gravitational waves in a hidden NJL sector","primary_cat":"hep-ph","submitted_at":"2026-04-21T08:07:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-field tunneling analysis in a CP-violating NJL model yields a slow transition (β/H ~ 100) whose stochastic gravitational-wave signal is detectable by μAres and insensitive to the CP angle.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Rel.26, 5 (2023), 2204.05434. [7] P. Amaro-Seoane et al. (LISA) (2017), 1702.00786. [8] T. Robson, N. J. Cornish, and C. Liu, Class. Quant. Grav.36, 105011 (2019), 1803.01944. [9] S. Babak, J. Gair, A. Sesana, E. Barausse, C. F. Sopuerta, C. P. L. Berry, E. Berti, P. Amaro- Seoane, A. Petiteau, and A. Klein, Phys. Rev. D95, 103012 (2017), 1703.09722. [10] P. A. Seoane et al. (LISA), Living Rev. Rel.26, 2 (2023), 2203.06016. [11] M. Colpi et al. (LISA) (2024), 2402.07571. [12] W.-R. Hu and Y.-L. Wu, Natl. Sci. Rev.4, 685 (2017). [13] J. Luo et al. (TianQin), Class. Quant. Grav.33, 035010 (2016), 1512.02076. [14] V. Corbin and N. J. Cornish, Class. Quant. Grav.23, 2435 (2006), gr-qc/0512039. 24 [15] J."},{"citing_arxiv_id":"2604.11903","ref_index":4,"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":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Based Gravitational-Wave Detectors, Living Rev. Rel. 16, 7 (2013), arXiv:1212.5575 [gr-qc]. [2] M. Evanset al., A Horizon Study for Cosmic Ex- plorer: Science, Observatories, and Community, (2021), arXiv:2109.09882 [astro-ph.IM]. [3] P. A. Seoaneet al.(LISA), Astrophysics with the Laser Interferometer Space Antenna, Living Rev. Rel.26, 2 (2023), arXiv:2203.06016 [gr-qc]. [4] I. Harry and J. Noller, Probing the speed of gravity with 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."},{"citing_arxiv_id":"2604.11893","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Relativistic signatures of scalar dark matter in extreme-mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Relativistic metric backreaction from scalar dark matter clouds in EMRIs produces dominant polar gravitational wave corrections for Mμ ≲ 0.12, exceeding axial and scalar radiation channels at small separations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"26, 331 (1971). [6] D. C. Robinson, Phys. Rev. Lett.34, 905 (1975). [7] V. Kalogera, B. Sathyaprakash, M. Bailes,et al., The Next Generation Global Gravitational Wave Observa- tory: The Science Book (2021), arXiv:2111.06990 [gr-qc]. [8] M. Colpi, K. Danzmann, M. Hewitson,et al.(LISA), LISA Definition Study Report (2024), arXiv:2402.07571 [astro-ph.CO]. [9] P. A. Seoane, J. Andrews, M. A. Sedda,et al. (LISA), Living Reviews in Relativity26, 2 (2023), arXiv:2203.06016 [gr-qc]. [10] P. Auclair, D. Bacon, T. Baker,et al.(LISA Cosmol- ogy Working Group), Living Reviews in Relativity26, 5 (2023), arXiv:2204.05434 [astro-ph.CO]. [11] K. Arun, E. Belgacem, R. Benkel,et al.(LISA), Living Reviews in Relativity25, 4 (2022), arXiv:2205."},{"citing_arxiv_id":"2604.06053","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Probing Kerr Symmetry Breaking with LISA Extreme-Mass-Ratio Inspirals","primary_cat":"gr-qc","submitted_at":"2026-04-07T16:41:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"tic GW backgrounds of cosmological origin generated by high-energy processes (around the TeV) in the early uni- verse; and (vi) unforeseen GW sources that may appear in this unexplored frequency window and for which we should be prepared. The LISA sources just described allow for a revo- lutionary science program [15] with strong impact in astrophysics [18], cosmology [19, 20], and fundamental physics [21-24], the latter being the focus of this work. In particular, we consider one of the GW sources that LISA will observe for the first time, namely EMRIs, to explore further their potential as high-precision probes of the nature of BHs. Specifically, EMRIs provide a unique opportunity to test whether BHs are well described by"},{"citing_arxiv_id":"2604.06009","ref_index":28,"ref_count":1,"confidence":0.9,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"How- ever, some progress may be achieved by working in the slow-rotation (low spin) approximation. Another promising direction is to extend our analy- sis to IMRIs, characterized by mass ratios in the range 10−4 ≲q≲10 −2 (see [79]). These systems may arise if IMBHs exist either in globular clusters or as companions to massive BHs in galactic nuclei [28]. Although IM- RIs typically produce shorter-duration signals than EM- RIs, their dynamics is more intricate, with spin-orbit and spin-spin couplings playing a more relevant role, with the spin of the secondary compact object contributing non- 6 negligibly. These effects will certainly introduce addi- tionalstructureinthegravitationalwaveform, whichmay"},{"citing_arxiv_id":"2511.16748","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"LISA as a probe of pre-big-bang physics: a nested sampling analysis","primary_cat":"gr-qc","submitted_at":"2025-11-20T19:01:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Nested sampling analysis indicates LISA could constrain H1, m, sigma_i and beta in the pre-big-bang model to relative uncertainties of about 18 percent under favorable conditions when including foregrounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.00307","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Spin-up and mass-gain in hyperbolic encounters of spinning black holes","primary_cat":"gr-qc","submitted_at":"2025-10-31T23:11:47+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Scattering black holes gain spin and mass by absorbing emitted gravitational radiation, with spin-up up to 0.3 and mass gain up to 15% in near-threshold encounters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.19047","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Global time-frequency search for stellar-mass binary black holes in LISA","primary_cat":"gr-qc","submitted_at":"2025-10-21T20:04:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A time-frequency semi-coherent search pipeline detects stellar-mass BBH inspirals in LISA data down to coherent SNR of approximately 11-14 on the Yorsh data challenge for aligned-spin, low-eccentricity systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.16113","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary","primary_cat":"gr-qc","submitted_at":"2025-10-17T18:00:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"centric equatorial inspirals into rapidly-spinning black holes, To be published (2025), arXiv:2506.09470 [gr- qc]. [29] O. Burke, G. A. Piovano, N. Warburton, P. Lynch, L. Speri, C. Kavanagh, B. Wardell, A. Pound, L. Durkan, and J. Miller, Assessing the importance of first postadiabatic terms for small-mass-ratio binaries, Phys. Rev. D109, 124048 (2024), arXiv:2310.08927 [gr- qc]. [30] P. Amaro-Seoaneet al.(LISA), Laser Interferometer Space Antenna, arXiv:1702.00786 [astro-ph.IM] (2017). [31] M. Colpiet al., LISA Definition Study Report, arXiv:2402.07571 [astro-ph.CO] (2024). [32] J. Luoet al.(TianQin), TianQin: a space-borne gravi- tational wave detector, Class. Quant. Grav.33, 035010 (2016), arXiv:1512.02076 [astro-ph.IM]. [33] E."},{"citing_arxiv_id":"2509.03360","ref_index":17,"ref_count":1,"confidence":0.9,"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":"2508.16399","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Constraints on the extreme mass-ratio inspiral population from LISA data","primary_cat":"gr-qc","submitted_at":"2025-08-22T14:00:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A neural-network-accelerated hierarchical Bayesian pipeline is developed and validated on a phenomenological model to constrain EMRI population parameters from LISA data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.22921","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Statistic threshold of distinguishing the environmental effects and modified theory of gravity with multiple massive black-hole binaries","primary_cat":"gr-qc","submitted_at":"2025-06-28T15:12:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The paper derives statistic thresholds to distinguish dynamical friction from dark matter spikes, extra dimension theory, and varying G theory using -4 PN order GW corrections in massive black hole binary inspirals across different astronomical models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2502.20166","ref_index":36,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Numerical simulations of density perturbation and gravitational wave production from cosmological first-order phase transition","primary_cat":"hep-ph","submitted_at":"2025-02-27T15:04:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"3D simulations of cosmological first-order phase transitions find density perturbation spectra with k^3 and k^{-1.5} slopes and GW spectra with k^3 and k^{-2}, confirming slow transitions can produce PBHs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2401.13668","ref_index":85,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Artificial Precision Timing Array: bridging the decihertz gravitational-wave sensitivity gap with clock satellites","primary_cat":"astro-ph.IM","submitted_at":"2024-01-24T18:59:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Proposes APTA with 6 satellites and 10^{-18} relative clock uncertainty at 1s averaging to achieve sensitivity for observing 10^3-10^4 solar-mass black hole mergers in the decihertz band.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Chakraborty, J. Cuadra, K. Dage, B. Davis, S. E. de Mink, R. Decarli, D. Doneva, S. Escoffier, P. Gandhi, F. Haardt, C. O. Lousto, S. Nissanke, J. Nordhaus, R. O'Shaughnessy, S. Portegies Zwart, A. Pound, F. Schussler, O. Sergi- jenko, A. Spallicci, D. Vernieri, and A. Vigna- G' omez, Living Reviews in Relativity26, 2 (2023), arXiv:2203.06016 [gr-qc]. [85] C. Ungarelli and A. Vecchio, Phys. Rev. D63, 064030 (2001). [86] A. J. Farmer and E. S. Phinney, Monthly No- tices of the Royal Astronomical Society346, 1197 (2003), https://academic.oup.com/mnras/article- pdf/346/4/1197/18649605/346-4-1197.pdf. [87] C. Cutler and D. E. Holz, Physical Review D80(2009), 10.1103/physrevd.80.104009. [88] T. Nakamura, M."},{"citing_arxiv_id":"2311.01300","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Waveform Modelling for the Laser Interferometer Space Antenna","primary_cat":"gr-qc","submitted_at":"2023-11-02T15:15:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of existing waveform models for LISA sources and the challenges that must still be overcome.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"section, we take an inventory of anticipated sources that need to be modelled to extract useful scientific results and are well-enough understood at this stage to be modelled in some detail. A more extensive survey of LISA's expected sources and the science that can be done with them can be found in the whitepaper produced by the LISA Astrophysics Working Group [3]. The short summaries here mainly focus on the expected parameter ranges to provide a context for the modelling approaches discussed in the rest of the white paper. Conventional long-lived astronomical sources include massive black hole binaries (MBHBs), extreme mass-ratio inspirals (EMRIs), intermediate mass-ratio inspirals (IMRIs), Galactic binaries (GBs) and stellar-origin"}],"limit":50,"offset":0}