{"total":26,"items":[{"citing_arxiv_id":"2605.21580","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18731","ref_index":110,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T17:53:13+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14264","ref_index":102,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The compact neutron star in 4U 1746-37 revisited: Reassessing the mass and radius","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T02:08:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Significant X-ray flux blocking in 4U 1746-37 allows the neutron star to have canonical mass and radius values of 1.59 solar masses and 13 km or 2.12 solar masses and 9.8 km.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09206","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Neutron stars in a conservative $f(R,T)$ gravity","primary_cat":"gr-qc","submitted_at":"2026-05-09T22:51:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A conservative f(R,T) gravity reformulation decouples the gravitational sector from the microphysical equation of state, enabling computation of neutron star mass-radius relations and tidal deformabilities that satisfy current astrophysical constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"star mergers, provides an important observational probe of deviations from General Relativity. By solving the stellar structure equations together with the differential equation governing the tidal Love number, we compute the mass-radius relations and tidal deformabilities predicted by the model and compare them with current astrophysical constraints from massive pulsars [1, 2], NICER measurements [5, 6], and gravitational-wave observations such as GW170817. II. CONSERVATIVEf(R, T)MODELS Several works in the literature attempt to construct energy-momentum conserved versions off(R, T) gravity by imposing the condition ∇µT µν = 0 (1) directly on the field equations in order to determine the functional form of the trace dependent functionh(T) in models of the form"},{"citing_arxiv_id":"2605.06418","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"On the non-radial oscillations of realistic anisotropic neutron stars: Axial modes","primary_cat":"gr-qc","submitted_at":"2026-05-07T15:26:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Axial modes of anisotropic neutron stars show mass-scaled frequency and damping time with nearly universal quadratic dependence on compactness, insensitive to EOS and anisotropy model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"arXiv:1304.6875 [astro-ph.HE]. [5] R. Abbott and et. al., GW170817: Observation of Grav- itational Waves from a Binary Neutron Star Inspiral, Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [6] N. Andersson and K. D. Kokkotas, Towards gravitational wave asteroseismology, Mon. Not. R. Astron. Soc.299, 1059 (1998), arXiv:gr-qc/9711088 [gr-qc]. [7] H. Heiselberg and V. Pandharipande, Recent Progress in Neutron Star Theory, Annu. Rev. Nucl. Part. Sci.50, 481 (2000), arXiv:astro-ph/0003276 [astro-ph]. [8] F. ¨Ozel and P. Freire, Masses, Radii, and the Equation of State of Neutron Stars, Annu. Rev. Astron. Astrophys 54, 401 (2016), arXiv:1603.02698 [astro-ph.HE]. [9] F. ¨Ozel, D. Psaltis, T. G¨ uver, G."},{"citing_arxiv_id":"2604.24949","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Physics Informed Bayesian Neural Network for the Neutron Star Equation of State","primary_cat":"astro-ph.HE","submitted_at":"2026-04-27T19:48:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A physics-informed Bayesian neural network learns neutron-star equations of state from theoretical priors and constraints, then generates posterior mass-radius and mass-tidal-deformability distributions consistent with NICER radii and 2-solar-mass limits.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Raaijmakerset al., The Astrophysical Journal Letters 918, L29 (2021), 2105.06981. [15] K. Zhouet al., Progress in Particle and Nuclear Physics 135, 104084 (2024), 2303.15136. [16] G. Papigkiotiset al., Physical Review D111, 083056 (2025), 2501.18544. [17] I. Liodis, E. Smyrniotis, and N. Stergioulas, Physical Review D109, 104008 (2024), 2309.03991. [18] Y. Fujimotoet al., Physical Review D110, 034035 (2024), 2401.12688. [19] N. Stergioulas, inCompact Objects in the Universe, edited by E. Papantonopoulos and N. Mavromatos (Cham, 2024) pp. 329-356. [20] S. Nget al., Classical and Quantum Gravity42, 205008 (2025), 2507.03232. [21] J.-J. Li, Y. Tian, and A. Sedrakian, Physical Review C 111, 055804 (2025), 2502."},{"citing_arxiv_id":"2604.11358","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Emulator-Assisted Nuclear DFT Inference and Its Consequences for the Structure of Neutron Stars","primary_cat":"nucl-th","submitted_at":"2026-04-13T11:55:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Emulator-assisted Bayesian inference of an extended Skyrme EDF, jointly constrained by nuclear observables, ab initio calculations, and NICER data, produces posteriors yielding consistent neutron star crust and core properties with a provided multivariate Gaussian for bulk nuclear matter parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.04560","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Neutron star with dark matter using vector portal","primary_cat":"hep-ph","submitted_at":"2026-04-06T09:40:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Vector portal fermionic dark matter admixed in neutron stars produces mediator-mass-dependent changes to the equation of state, yielding distinct mass-radius relations and tidal deformabilities that observations can use to constrain the model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"from Magnetars,JHEP06(2018) 048, [arXiv:1804.01992]. [54] C. H. Lenzi, M. Dutra, O. Louren¸ co, L. L. Lopes, and D. P. Menezes,Dark matter effects on hybrid star properties,Eur. Phys. J. C83(2023), no. 3 266, [arXiv:2212.12615]. [55] C. Kouvaris and P. Tinyakov,Can Neutron stars constrain Dark Matter?,Phys. Rev. D82 (2010) 063531, [arXiv:1004.0586]. [56] H. Sotani and A. Kumar,Universal relation involving fundamental modes in two-fluid dark matter admixed neutron stars,Eur. Phys. J. C85(2025), no. 12 1438, [arXiv:2512.07105]. [57] A. Issifu, P. Thakur, D. Rafiei Karkevandi, F. M. da Silva, D. P. Menezes, Y. Lim, and T. Frederico,Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach,arXiv:2511."},{"citing_arxiv_id":"2604.02782","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Spin effects in superfluidity, neutron matter and neutron stars","primary_cat":"astro-ph.HE","submitted_at":"2026-04-03T06:47:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"13(1964) 789-791. [11] P. Demorest, T. Pennucci, S. Ransom, M. Roberts and J. Hessels,Shapiro Delay Measurement of A Two Solar Mass Neutron Star,Nature467(2010) 1081-1083, [1010.5788]. [12]NANOGravcollaboration, Z. Arzoumanian et al., The NANOGrav 11-year Data Set: High-precision timing of 45 Millisecond Pulsars,Astrophys. J. Suppl. 235(2018) 37, [1801.01837]. [13] H. T. Cromartie et al.,Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar,Nature Astron.4(2019) 72-76, [1904.06759]. [14] J. Antoniadis, P. C. Freire, N. Wex, T. M. Tauris, R. S. Lynch et al.,A Massive Pulsar in a Compact Relativistic Binary,Science340(2013) 6131, [1304.6875]. [15] E. Fonseca et al.,Refined Mass and Geometric"},{"citing_arxiv_id":"2602.06696","ref_index":88,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian Constraints on the Neutron Star Equation of State with a Smooth Hadron-Quark Crossover","primary_cat":"nucl-th","submitted_at":"2026-02-06T13:34:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of a smooth hadron-quark crossover EOS finds current observations tightly constrain the density dependence of nuclear symmetry energy while leaving highest-density hadronic and quark-matter parameters only weakly constrained.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.07931","ref_index":34,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly","primary_cat":"gr-qc","submitted_at":"2026-01-12T19:01:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.24194","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of Anisotropy on Neutron Star Structure and Curvature","primary_cat":"gr-qc","submitted_at":"2025-12-30T12:53:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.02484","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Properties of Stable Massive Quark Stars in Holography","primary_cat":"hep-ph","submitted_at":"2025-12-02T07:18:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Holographic model of massive deconfined quarks yields a stiff enough equation of state to allow stable 2-solar-mass hybrid stars with quark cores for certain nuclear phases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.01503","ref_index":79,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian inferences on covariant density functionals from multimessenger astrophysical data: Influences of parametrizations of density dependent couplings","primary_cat":"astro-ph.HE","submitted_at":"2025-12-01T10:27:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Different parametrizations of density dependence in covariant density functionals produce significant variations in the high-density equation of state and symmetry energy, with rational-function forms providing flexibility when saturation properties are adjusted and constrained by multimessenger ast","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.18681","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tracing the Trace Anomaly of Dense Matter inside Neutron Stars","primary_cat":"astro-ph.HE","submitted_at":"2025-11-24T01:45:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Quasi-universal relations connect the trace anomaly profile of neutron star matter to stellar compactness, moment of inertia, and tidal deformability, yielding a central value estimate of Δ_c = 0.1770^{+0.0365}_{-0.0432} for a 1.4 M_⊙ star.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.22137","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inferring neutron-star Love-Q relations from gravitational waves in the hierarchical Bayesian framework","primary_cat":"gr-qc","submitted_at":"2025-10-25T03:18:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.13322","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities","primary_cat":"hep-ph","submitted_at":"2025-09-16T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In contrast, the heavier models reach up to 60 MeV and are therefore representative of the hotter end of the spectrum. In the model names, numbers such as 18.8 denote the progenitor star's mass in solar units. - 17 - The first letters of the model names denote the used EoS. The SFHo one [76] is fully compatible with all current constraints from nuclear theory and experiment [77-79] as well as astrophysics, including pulsar mass measurements [80-82] and the radius constraints deduced from gravitational-wave and Neutron Star Interior Composition Explorer mea- surements [83-85]. Results for the long-used LS220 EoS [86] are shown for comparison. These EoS are considerably softer than what was popular earlier, but the stiff variants"},{"citing_arxiv_id":"2509.06145","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Equation of State Extrapolation Systematics: Parametric vs. Nonparametric Inference of Neutron Star Structure","primary_cat":"astro-ph.HE","submitted_at":"2025-09-07T17:21:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Nonparametric GP-based high-density extensions yield softer EOS posteriors with larger uncertainties than parametric PP extensions when jointly constrained by multi-messenger neutron star observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.15912","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"$f$-mode Oscillations for Hyperons and H-dibaryons in Neutron Stars","primary_cat":"astro-ph.HE","submitted_at":"2025-08-21T18:18:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The study examines the effects of hyperons and H-dibaryons on f-mode oscillations in neutron stars using the quark meson coupling model and tests universal relations in the Cowling approximation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.16929","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Properties of the neutron star crust informed by nuclear structure data","primary_cat":"nucl-th","submitted_at":"2025-05-22T17:22:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bayesian NS EoS study using full nuclear posterior distributions and consistent crust modeling finds increased surface thickness and crustal moment of inertia relative to prior work.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04654","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Phase transitions in neutron stars and their links to gravitational waves","primary_cat":"astro-ph.HE","submitted_at":"2019-07-05T19:07:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"are extremely precisely determined from their orbital parameters. NSs masses tend to concentrate around the canonical 1.4 M ⊙ but the most stringent observational constraints on the NS EoS arise from two pulsating NSs in binary systems with white dwarfs companions: PSR J1614-2230 [13] with M = 1.908± 0.016 M ⊙ [16], and PSR J0348+0432, with M = 2.01± 0.04 M⊙ [15]. These highly precise measurements based on timing analysis, challenge the high-density EoS models, but also impose limits on the EoS at lower densities (see figure 6 in section 5). On the other hand, NSs spin can be precisely determined either from pulsar radio or X-ray timing obser- vations. A theoretical NS maximum spin frequency is given by the Kepler limit."},{"citing_arxiv_id":"1907.06597","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hot quark matter and (proto-) neutron stars","primary_cat":"nucl-th","submitted_at":"2019-07-05T16:10:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"An extended PNJL model locates the QCD critical end point and predicts that proto-neutron stars contain hyperons and Delta-isobars but no deconfined quarks, which appear only in cold neutron stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.03549","ref_index":46,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Anisotropic strange quark stars with a non-linear equation-of-state","primary_cat":"gr-qc","submitted_at":"2019-07-05T10:16:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Exact analytical solution for anisotropic CFL strange quark stars with non-linear EOS, satisfying energy conditions, yielding mass-radius profiles and compactness values.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.10791","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining the scalar-tensor gravity theories with and without screening mechanisms by combined observations","primary_cat":"gr-qc","submitted_at":"2019-06-26T00:27:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Combined Cassini, LLR, and pulsar observations tighten bounds on scalar-tensor gravity with and without screening, with LLR improving SMG limits by over seven orders of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.10316","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining light fermionic dark matter with binary pulsars","primary_cat":"astro-ph.GA","submitted_at":"2019-06-25T04:15:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dynamical friction from a degenerate fermionic dark matter background induces measurable secular decay in binary pulsar orbital periods, with sensitivity to fermion masses ≳50 eV and example upper bounds around 1 keV from Milky Way data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1904.05363","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Testing the nature of dark compact objects: a status report","primary_cat":"gr-qc","submitted_at":"2019-04-10T18:00:05+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Current and future observations can test whether dark compact objects are Kerr black holes or exotic alternatives, with null results strengthening the black hole paradigm.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"An increase in sensitivity of current detectors and the advent of next-generation interfer- ometers on ground and in space will open the frontier of precision GW astrophysics. GWs are produced by the coherent motion of the sources as a whole: they are ideal probes of strong gravity, and play the role that EM waves did to test the Rutherford model. In parallel, novel techniques such as radio and deep infrared interferometry [8, 9] are now providing direct images of the center of ours and others galaxies, where a dark, massive and compact object is lurking [10-14]. The wealth of data from GW and EM observations has the potential to inform us on the following outstanding issues: 1.2 Problems on the horizon Classically, spacetime singularities seem to be always cloaked by horizons and hence inac-"}],"limit":50,"offset":0}