{"total":25,"items":[{"citing_arxiv_id":"2605.20509","ref_index":69,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Causal Bootstrap: Bounding Smeared Spectral Functions from Non-Perturbative Euclidean Data","primary_cat":"hep-lat","submitted_at":"2026-05-19T21:25:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The causal bootstrap computes rigorous bounds on smeared spectral functions from non-perturbative Euclidean data by optimizing over the convex set of compatible positive spectral densities and reducing dual problems to semidefinite programs for certain kernels.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19571","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"From mass-loss histories to lightcurves: a generalised framework for interaction-powered transients","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T09:17:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Introduces a generalized fast framework for modeling interaction-powered transients with arbitrary CSM profiles and multi-wavelength outputs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17318","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"RooAgent: An LLM Agent for Root-Based High Energy Physics Analysis","primary_cat":"hep-ph","submitted_at":"2026-05-17T08:20:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"RooAgent provides an LLM agent interface that translates natural-language prompts into calls to PyROOT analysis functions for high energy physics tasks, with support for multiple AI backends and tested on ZH simulations and ATLAS open data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11703","ref_index":179,"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":"120] andpSEOBNR [126-130] tests implemented in Bil- byTGR [169], as well as with the QNMRF [131-134] and ringdown[135-137] pipelines. Cosmological inference was performed with thegwcosmo[170-172] andicarogw[173, 174] codes. Some of the parameter-estimation analysis were managed with the Asimovlibrary [175]. Plots were pre- pared with Matplotlib[176],seaborn[177] and GWpy[178]. NumPy[179] and SciPy[180] were used in the preparation of the manuscript. C01 strain data for GW240925 and C00 strain data for GW250207 analysed as part of this study are publicly available through Gravitational Wave Open Science Cen- ter (GWOSC) [181]; the (miscalibrated) C00 strain data for GW240925 are available in a supplemental release from Zen- odo. Data releases of inference results, together with example"},{"citing_arxiv_id":"2605.10768","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Unitaria: Quantum Linear Algebra via Block Encodings","primary_cat":"quant-ph","submitted_at":"2026-05-11T16:00:15+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Unitaria is a new open-source Python library that provides a high-level, composable interface for block encodings in quantum computing, enabling automatic circuit generation and classical simulation-based verification.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"processors throughAQT[ 37] orQiskit[ 17], as well as simulators likeQulacs[ 22], which is used as the default simulator, orCUDA-Q[ 23]. The software architecture is designed to allow support for other backends (such asQrisporPennyLane) in the future. Only core operations build circuits directly, allowing easy integration of other circuit backends. For classical calculations,Unitaria usesNumPy[38] andSciPy[39]. 4 Examples In this section, we demonstrate the usage ofUnitariathrough code examples. We start with the basic usage of Node objects and then turn to two practical examples, namely the solution of a partial differential equation and the implementation of convolutions. 4.1 A simple increment circuit As a basic usage demonstration, let us look at theIncrement node, which implements the (unitary)"},{"citing_arxiv_id":"2605.08080","ref_index":105,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"CMB Limits on the Absorption of Light Vector and Axial-Vector Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-05-08T17:59:28+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Planck CMB data set upper limits on vector and axial-vector dark matter-electron couplings for masses 100 eV to 100 keV via energy injection from inelastic scattering and hydrogen absorption.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07779","ref_index":59,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Neural network quantum states in the grand canonical ensemble","primary_cat":"quant-ph","submitted_at":"2026-05-08T14:18:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new neural quantum state ansatz for bosons in the grand canonical ensemble achieves competitive variational energies in 1D and 2D systems and provides access to one-body reduced density matrices.","context_count":1,"top_context_role":"other","top_context_polarity":"unclear","context_text":"manipulation and automatic differentiation. Neural net- work design was conducted using Flax [54]. Optax [55] was used for optimization. NumPy [56] and SciPy [57] were utilized for data processing, and plots were pro- duced using Matplotlib [58]. The codes used to run the simulations and reproduce the examples presented in this paper are available on GitHub in Ref. [59]. [1] Adolfo Avella and Ferdinando Mancini, eds., Strongly Correlated Systems: Numerical Methods , Springer Series in Solid-State Sciences, Vol. 176 (Springer, Berlin, Hei- delberg, 2013). [2] Juan Carrasquilla and Giacomo Torlai, \"How To Use Neural Networks To Investigate Quantum Many-Body Physics,\" PRX Quantum2, 040201 (2021). [3] GiuseppeCarleoandMatthiasTroyer,\"Solvingthequan-"},{"citing_arxiv_id":"2605.03947","ref_index":92,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Effects of magnetically driven shocks on nucleosynthesis and kilonovae from neutron star mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-05-05T16:32:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Magnetically driven shocks from neutron star merger remnants can reheat ejecta to nuclear statistical equilibrium, alter r-process yields, and produce observable changes in kilonova color and light curves.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"tions were performed on the NERSC Perlmutter clus- ter through allocations m4575 and m5081. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Con- tract No. DE-AC02-05CH11231. Software used in this work includeskuibit[90], matplotlib [91], numpy [92], and scipy [93]. [1] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [2] B. P. Abbottet al.(LIGO Scientific, Virgo, Fermi GBM, INTEGRAL, IceCube, AstroSat Cadmium Zinc Telluride Imager Team, IPN, Insight-Hxmt, ANTARES, Swift, AGILE Team, 1M2H Team, Dark Energy Camera GW-EM, DES, DLT40, GRAWITA, Fermi-LAT, ATCA,"},{"citing_arxiv_id":"2604.21010","ref_index":77,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravity Echoes from Supermassive Black Hole Binaries","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T19:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Future microhertz detections combined with nanohertz pulsar terms can serve as gravity echoes to measure supermassive black hole binary inspiral rates from hundreds to thousands of years in the past.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"this manuscript, the authors became aware of concurrent work by Criswell et al. (in prep) on pulsar terms in the post-merger regime. SOFTW ARE This work made use ofhasasia[31, 33] for PTA sen- sitivity curve computation and deterministic continuous- wave signal-to-noise ratio estimates,gwent[37] for multi- band detector noise modeling,NumPy[74],SciPy[75], Matplotlib[76], andStreamlit[77] for the inter- active sensitivity visualization. The post-Newtonian evolution library and the multiband sensitivity dash- boardapp.pyare available athttps://github.com/ ChiaraMingarelli/gravity-echoes. A hosted ver- sion of the interactive dashboard is athttps:// gravityecho.streamlit.app. Codes were written and edited with the assistance of Claude Code (Anthropic)."},{"citing_arxiv_id":"2604.19922","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Measuring neutrino mass and asymmetry through galaxy pairwise peculiar velocity","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T19:01:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Galaxy pairwise peculiar velocities from Cosmicflows-4 yield M_ν = 0.24^{+0.34}_{-0.18} eV and η² = 2.14^{+0.30}_{-0.32} (7σ non-zero asymmetry) in the CMB framework, consistent with prior Planck results.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16600","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A data-driven prediction for the primordial deuterium abundance","primary_cat":"astro-ph.CO","submitted_at":"2026-04-17T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Gaussian process regression on nuclear data predicts 10^5 D/H = 2.442 ± 0.040, 1.70 sigma below observation and consistent with first-principles calculations.","context_count":1,"top_context_role":"other","top_context_polarity":"unclear","context_text":"In addition, T.L. and H.L. are supported by the Cecile K. Dalton Career Development Professorship, endowed by Boston Univer- sity trustee Nathaniel Dalton and Amy Gottleib Dalton. C.G. is supported by the Office of High Energy Physics of the U.S. Department of Energy under contract DE-AC02- 05CH11231. This work makes use of matplotlib [39], JAX [40], NumPy [41], SciPy [42], and MINUIT [43]. [1] E. Averet al., \"The LBT Y P Project IV: A New Value of the Primordial Helium Abundance\", (2026), arXiv:2601.22238 [astro-ph.CO]. [2] T.-H. Yehet al., \"The LBT Y P Project V: Cosmological Implications of a New Determination of Primordial 4He\", (2026), arXiv:2601.22239 [astro-ph.CO]. [3] N. Aghanimet al.(Planck Collaboration), \"Planck 2018"},{"citing_arxiv_id":"2604.13687","ref_index":52,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09283","ref_index":100,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Probing Solar Symmetrons with Direct Detection","primary_cat":"hep-ph","submitted_at":"2026-04-10T12:54:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Solar tachocline production of symmetrons yields a keV-scale flux at Earth whose absorption in xenon detectors provides new complementary bounds on symmetron parameter space.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"12350610240\"AstrophysicalAxionLaboratories\", and the State Key Laboratory of Dark Matter Physics at Shanghai Jiao Tong University. L.V. additionally thanks the Tsung-Dao Lee Institute and the Xplorer Symposia Organization Committee of the New Cornerstone Science Foundation for hospitality during the final stages of this work. This work made use of the open source software matplotlib [99], numpy [100], and scipy [101]. Appendix A: Derivation of the production rate The calculation of the production rate proceeds via the finite-temperature field theory relation between the imaginary part of the scalar self-energyΠϕ and the emis- sion rate. The photon propagating in the solar plasma is described by the polarization tensor Πµν(ω,k) = Π T (ω, k)P µν"},{"citing_arxiv_id":"2602.13232","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"PlotChain: Deterministic Checkpointed Evaluation of Multimodal LLMs on Engineering Plot Reading","primary_cat":"cs.AI","submitted_at":"2026-01-29T06:08:19+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"PlotChain benchmark reports top MLLMs reaching ~80% field-level accuracy on engineering plot reading under human-like tolerances, but with persistent failures on frequency-domain tasks like bandpass and FFT spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.25886","ref_index":83,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mitigating gain calibration errors from EoR observations with SKA1-Low AA*","primary_cat":"astro-ph.CO","submitted_at":"2025-10-29T18:33:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show hybrid foreground mitigation (GPR + PCA combined with avoidance) recovers the HI 21cm signal within 2σ for gain calibration errors ≤1% in SKA1-Low AA* observations over 0.05-0.5 Mpc^{-1} scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.04332","ref_index":143,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Biased parameter inference of eccentric, spin-precessing binary black holes","primary_cat":"gr-qc","submitted_at":"2025-10-05T19:29:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Eccentric BBH signals recovered with quasi-circular precessing models show biases in chirp mass and χ_p; Bayes factors favor eccentric aligned-spin models when both eccentricity and precession are present.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Numerical relativity sim- ulations and some parameter estimation runs were per- formed on thesonicHPC at ICTS-TIFR. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants Np. PHY-0757058 and No. PHY- 0823459. We used the following software packages: LALSuite[141],PyCBC[142],bilby[126],NumPy[143], Matplotlib[144],Seaborn[145],jupyter[146], dynesty[147],corner[148]. This document has LIGO preprint numberLIGO-P2500606. Appendix A: Priors used for parameter estimation The priors on various parameters used for non- spinning, aligned-spin, and precessing-spin analyses are listed in Table III. Parameter Prior Range M Uniform in component masses"},{"citing_arxiv_id":"2509.23123","ref_index":47,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Constraining Inflationary Particle Production with CMB Polarization","primary_cat":"astro-ph.CO","submitted_at":"2025-09-27T05:04:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"No evidence for primordial hotspots in Planck polarization data leads to improved bounds on inflationary particle production couplings for light particles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.13654","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cosmic Birefringence from the Atacama Cosmology Telescope Data Release 6","primary_cat":"astro-ph.CO","submitted_at":"2025-09-17T02:59:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of ACT DR6 CMB polarization data measures cosmic birefringence angle β = 0.215° ± 0.074° excluding zero at 2.9σ, consistent with prior WMAP and Planck results but limited by unexplained systematics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.03458","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Comparison of Halo Model and Simulation Predictions for Projected-Field Kinematic Sunyaev-Zel'dovich Cross-Correlations","primary_cat":"astro-ph.CO","submitted_at":"2025-09-03T16:33:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Halo model predictions match Websky simulations well for Planck filters but differ by ~20% for Simons Observatory filters, exceeding error bars and consistent with missing higher-order terms in the kSZ signal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.22363","ref_index":59,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Binary black holes in the heat of merger","primary_cat":"gr-qc","submitted_at":"2025-06-27T16:25:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Develops a frequency-domain approximant for tidal heating in nonspinning black hole binaries that extends to merger and includes horizon parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.14529","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Search for Dark Matter in 2HDMS at LHC and future Lepton Colliders","primary_cat":"hep-ph","submitted_at":"2025-04-20T08:03:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Benchmarks in the 2HDMS model with light to heavy dark matter masses are identified under all constraints and shown to have better discovery prospects at future lepton colliders than at the HL-LHC via cut-and-count analyses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.16103","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Validating Prior-informed Fisher-matrix Analyses against GWTC Data","primary_cat":"gr-qc","submitted_at":"2024-04-24T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Fisher-matrix methods in GWFish match LIGO/Virgo posteriors reasonably when priors are included, with prior impact scaling with parameter degeneracy, supporting their use for ET forecasts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2112.06861","ref_index":281,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with GWTC-3","primary_cat":"gr-qc","submitted_at":"2021-12-13T18:19:04+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"No evidence for physics beyond general relativity is found in the analysis of 15 GW events from GWTC-3, with consistency in residuals, PN parameters, and remnant properties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"devising new tests or improving the existing ones, optimizing their sensitvity to predictions from specific modified theories of gravity, can play a very important role in constraining beyond- GR physics using future gravitational-wave observations. ACKNOWLEDGMENTS Analyses in this paper made use of NumPy [275], SciPy [276], Astropy [277, 278], IPython [279], qnm [280], PE- Summary [281], and GWpy [282]; plots were produced with Matplotlib[283], and Seaborn [284]. Posteriors were sampled with Stan [285], CPNest [146], PyMultinest [286, 287], Bilby [138, 139], and LALInference [140]. Power spectral densities are generated through the software BAYESWAVE [84, 147]. This material is based upon work supported by NSF's LIGO Labo- ratory which is a major facility fully funded by the National"},{"citing_arxiv_id":"2111.03606","ref_index":165,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2021-11-05T16:43:17+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GWTC-3 catalogs 90 compact binary coalescence events with p_astro > 0.5 from LIGO and Virgo's first three observing runs, including the first confident neutron star-black hole binaries.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"low-likelihood peaks describe the sources (assuming that the signals are astrophysical). All results are given assuming our default pri- ors. We highlight results for GW200308 173609 and GW200322 091133 in Table IV and the figures to indicate that these results may be especially sensitive to the choice of prior. Using a different prior, such as a population- informed prior [116, 119, 165-169], that has a stronger preference for masses more consistent with other GW ob- servations, and a weaker preference for high masses and large distances, would alter results. A. Masses Masses are typically the best constrained binary pa- rameters. They are the dominant properties in setting the frequency evolution of the signal, with lower- (higher- ) mass systems merging at higher (lower) frequencies."},{"citing_arxiv_id":"2010.14529","ref_index":276,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2020-10-27T18:01:34+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No evidence for deviations from general relativity is found in LIGO-Virgo binary black hole events, with improved constraints on waveform parameters, graviton mass, and ringdown properties.","context_count":1,"top_context_role":"other","top_context_polarity":"unclear","context_text":"agreements that would be indiscernible from individual signals. With constantly improving detectors and analysis capabilities, we will continue to expand the scope and sensitivity of our tests of GR and our probes of the nature of BHs when analyzing data from O3b and future observing runs. ACKNOWLEDGMENTS Analyses in this paper made use of NumPy[ 271], SciPy [272], Astropy[ 273, 274], IPython[ 275],qnm[ 276], PE- Summary[ 277], and GWpy[ 278]; plots were produced with Matplotlib[ 279], and Seaborn[ 280]. Posteriors were sam- pled with Stan[ 128], CPNest[ 281], PyMultinest[ 282, 283], and LALInference[ 116]. The authors gratefully acknowledge the support of the United States National Science Founda- tion (NSF) for the construction and operation of the LIGO"}],"limit":50,"offset":0}