{"total":46,"items":[{"citing_arxiv_id":"2607.02498","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Alleviating prior dependencies for DESI DR1 clustering fits through reparameterization","primary_cat":"astro-ph.CO","submitted_at":"2026-07-02T17:57:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Jeffreys prior over EFTofLSS coefficients mitigates projection effects in DESI DR1 power spectrum multipole fits, recentering posteriors for late-time expansion parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.01226","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T17:57:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Dynamical dark energy remains preferred across extended models while curvature, neutrino mass and inflation parameters show strong model dependence, with no resolution of the H0 tension.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"86(2001) 3475 [astro-ph/0007333]. [16]WMAPcollaboration,Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results,Astrophys. J. Suppl.208(2013) 20 [1212.5225]. [17]WMAPcollaboration,Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Parameter Results,Astrophys. J. Suppl.208(2013) 19 [1212.5226]. [18]Planckcollaboration,Planck 2018 results. I. Overview and the cosmological legacy of Planck,Astron. Astrophys.641(2020) A1 [1807.06205]. [19]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys. 641(2020) A6 [1807.06209]. [20]ACTcollaboration,The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth,Astrophys."},{"citing_arxiv_id":"2607.00785","ref_index":111,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Assembly bias and the redshift evolution of intrinsic alignments for LRGs","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T11:15:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FLAMINGO simulation analysis shows IA amplitude for LRGs depends on halo assembly history and exhibits redshift evolution beyond mass effects, yielding an empirical mass-redshift model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.00610","ref_index":295,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Correcting the hydrostatic mass for non-thermal gas motions: a comparison of two approaches","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T08:35:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The two correction approaches differ in their radial dependence in 3D but agree to within a few percent in projected observations, with the non-thermal pressure fraction underestimated by a factor of about 2.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31977","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining dark energy with complementary probes of large-scale structure","primary_cat":"astro-ph.CO","submitted_at":"2026-06-30T17:17:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Adding DESI DR1 RSD, DES Y3 3x2pt, and ISW cross-correlations to CMB+BAO+SNe improves FoM for EFTofDE parameters {cB, cM} by 2.69x and for {mu(z), Sigma(z)} by 3.37x, with 2.9 sigma deviation from LambdaCDM similar to w0waCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27714","ref_index":102,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Fast Radio Bursts as Cosmological Probes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T04:44:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"FRBs serve as cosmological probes via dispersion measure, scattering, and Faraday rotation to constrain baryon distribution, expansion history, magnetic fields, and fundamental physics effects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25583","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Weak Lensing with SKAO: Cosmic Shear Cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T08:56:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts indicate SKAO cosmic shear can constrain S8 to 5% alone and 3% combined with LSST or Euclid, with added benefits from polarization and kinematics for separating lensing signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23651","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the 'Lensing is Low' Problem with UNIONS","primary_cat":"astro-ph.CO","submitted_at":"2026-06-22T17:36:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New UNIONS galaxy-galaxy lensing data around CMASS galaxies indicates no significant lensing is low problem, with joint HOD fits to GGL and GC favoring a slightly lower matter power spectrum amplitude than Planck.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21826","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Energy in the DESI Era: A Brief Review of Evidence, Beyond-$\\Lambda$CDM Interpretations, and Tensions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-20T01:29:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review of DESI evidence for dynamical dark energy, its dependence on parametrization and datasets, and alternative beyond-LambdaCDM interpretations that may address cosmological tensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20036","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evolving Dark Energy Is Vacuum Energy After All","primary_cat":"astro-ph.CO","submitted_at":"2026-06-18T10:10:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A QCD-vacuum-based model of dynamical dark energy fits Planck+ACT+SPT, DESI DR2, and supernova data while reproducing the late-time evolution favored by DESI.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19090","ref_index":137,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resolving the Hubble Tension in the Early Dark Energy Framework with JWST and DESI Data","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T13:58:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Axion EDE model fitted to Planck/ACT/SPT CMB, DESI BAO, and JWST UV luminosity function data yields H0 = 71.58 ± 1.05 km s^{-1} Mpc^{-1}, reduces H0 tension to 1.0 sigma, and improves Δχ^{2}_tot = -18.26 over Λ CDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18437","ref_index":180,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of inhomogeneous curvature on growth rate measurements from magnitude fluctuations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-16T19:40:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Full-GR simulations find that inhomogeneous curvature produces only sub-dominant systematic offsets in growth-rate measurements from magnitude fluctuations at z ≲ 0.2 relative to current statistical errors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12521","ref_index":43,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Matter with a Drag at Low Redshift","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"iDCDM adds two parameters to LambdaCDM so that dark matter decay produces late-time interacting radiation, yielding a distinctive low-redshift suppression of structure growth while leaving BBN and primary CMB unchanged.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12255","ref_index":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Towards Practical Field-Level Inference for Weak Lensing","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T15:57:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Field-level inference from weak lensing maps yields significantly tighter cosmological constraints than power-spectrum analysis when using the same forward-modeling pipeline, especially on small scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11368","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Non-linear Structure Formation in Planck+DESI Favoured Interacting Dark Energy Cosmologies","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T18:49:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"N-body simulations of IDE with Q=ξHρ_x show scale-dependent deviations in the matter power spectrum, density morphology, and halo abundance that standard ΛCDM-calibrated prescriptions cannot reproduce.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06495","ref_index":171,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"What it takes to solve the Hubble tension through Modifications of Cosmological Recombination II: in light of ACT DR6 and DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Perturbative modifications to the electron mass m_e(z) resolve the Hubble tension with Planck+ACT CMB data but cannot when DESI DR2 BAO data are added due to lowered Omega_m.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"S8 = 0.798 +0.014 −0.015 [169].7 However, as in Paper I, the model is less consistent with late-time probes of Ω m: the increase inH 0 at fixed Ω mh3, which controls the angular scale of the sound horizon, requires a decrease in Ω m, somewhat lower than the DESI DR2 constraint [143] and inconsistent with the PantheonPlus constraint Ωm = 0.334±0.018 [171]. This is the same fundamental limitation identified in Paper I, and motivates the inclu- sion of BAO data in the following subsection. 6 SinceS 8 is a derived parameter, its uncertainty is estimated via linear error propagation through the Fisher matrix, as described in Appendix D. 7 We note, however, that the current status of theS 8 tension is subject to debate: KiDS Legacy finds consistency with the CMB"},{"citing_arxiv_id":"2606.06410","ref_index":59,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Atacama Cosmology Telescope: Probing new signatures of ultralight axions with gravitational lensing","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T17:14:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New upper limits on ultralight axion dark matter fraction (<1.5% at 10^{-26} eV, <9% at 10^{-25} eV at 95% CL) from combined CMB lensing data, plus marginal 2.1σ preference at 10^{-24.5} eV driven by few points.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05853","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reconstructing dark energy with fewer assumptions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T08:27:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bin-wise uncorrelated reconstruction from DESI/SDSS BAO and Pantheon+/Union3.1/DES-Dovekie supernovae yields dark energy density peaking then declining and equation of state oscillating with phantom crossing near z~0.7, consistent across datasets at moderate significance.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05479","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the potential for inhomogeneities to mimic an evolving dark energy","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T21:57:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Numerical simulations show that inhomogeneities in a LambdaCDM universe can lead some observers to infer evolving dark energy parameters consistent with DESI at 2-sigma.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27221","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Dynamical Dark Energy from Multiple Probes in the Full Dark Energy Survey","primary_cat":"astro-ph.CO","submitted_at":"2026-05-26T16:08:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Full DES data from SN+BAO+3x2pt yields w0=-0.84, wa=-0.44 with 2.2σ deviation from ΛCDM; adding DESI+CMB reaches 3.0σ while 3x2pt improves figure of merit by ~10%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.26116","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-25T17:59:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Any unified early and late dark energy scenario with a single tracking scalar field requires a potential with three distinct slopes arranged in a steep-steeper-shallow hierarchy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Gong,The evidence of cosmic acceleration and observational constraints, JCAP06(2020) 059 [1912.07375]. [9] E. Di Valentino, S. Gariazzo, O. Mena and S. Vagnozzi,Soundness of Dark Energy properties, JCAP07(2020) 045 [2005.02062]. [10] S. Nadathur, W.J. Percival, F. Beutler and H. Winther,Testing Low-Redshift Cosmic Acceleration with Large-Scale Structure,Phys. Rev. Lett.124(2020) 221301 [2001.11044]. [11] B.M. Rose, D. Rubin, A. Cikota, S.E. Deustua, S. Dixon, A. Fruchter et al.,Evidence for Cosmic Acceleration is Robust to Observed Correlations Between Type Ia Supernova Luminosity and Stellar Age,Astrophys. J. Lett.896(2020) L4 [2002.12382]. [12]DES, SPTcollaboration,Cosmological constraints from DES Y1 cluster abundances and SPT multiwavelength data,Phys."},{"citing_arxiv_id":"2605.23841","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"cloelike: A Python Library for Cosmological Likelihood Inference in the Euclid Era","primary_cat":"astro-ph.CO","submitted_at":"2026-05-22T16:50:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"cloelike is a new open Python package implementing composable Gaussian likelihoods for WL, GCph, GGL, full-shape spectra, and BAO in joint probe combinations for Euclid analyses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23839","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"cloelib: A Flexible Python Library for Computing Cosmological Observables in the Euclid Era","primary_cat":"astro-ph.CO","submitted_at":"2026-05-22T16:48:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"cloelib is a modular JAX-based Python library for cosmological observables intended as reference infrastructure for Euclid's first data release.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22309","ref_index":95,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Signatures of Modified Gravity Below $\\mathcal{O}(10)$ Mpc in a Dynamical Dark Energy Background","primary_cat":"astro-ph.CO","submitted_at":"2026-05-21T10:55:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Modified gravity below O(10) Mpc in a CPL dynamical dark energy background is required to suppress structure growth at low redshifts while satisfying CMB constraints from ISW and lensing.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"within the ΛCDM model, such as the growth tension. In particular, data from redshift-space distortions (RSD) and weak gravitational lensing typically favor a lower level of structure formation than that predicted not only by the best-fit ΛCDM model from the Planck analy- sis, but also by the quintom scenario mentioned above [82-93] (see, however, [94]). Although a larger neutrino mass [95] or interactions in the dark sector (see, e.g., [63, 85, 96-99]) can reduce the tension at some extent, it could also be an indication of modified gravity (MG) effects at cosmological scales. In thisLetter, we investigate such a possibility con- sidering both dynamical DE through the Chevallier- Polarski-Linder (CPL) form of the equation-of-state (EoS) parameter [100, 101],w(a) =w 0 +w a(1−a), -"},{"citing_arxiv_id":"2605.15078","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"KiDS+VIKING-450 cosmology with Bayesian hierarchical model redshift distributions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T17:02:28+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian hierarchical modeling of photometric redshifts in KiDS+VIKING-450 raises S8 to 0.756 ± 0.039 and reduces Planck tension to 1.9σ.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"ˆFb ∼N(aF b,σ 2 b ),(1) whereσ 2 b is the flux variance of the galaxy in bandb, andais an am- plitude.F b is the noise-free flux, given by integrating the redshifted rest-frame template spectrumL t (ν)multiplied by the filter response MNRAS000, 1-14 (2026) KV450 cosmology with BHM n(z)3 Wb(ν)over frequency, Fb(t,z) = 1+z 4πD2 L(z) Z ∞ 0 dν ν Lt (ν)[ν(1+z)]W b(ν),(2) whereD L(z)is the luminosity distance. Note that the templates have an arbitrary normalisation, so an amplitudeais introduced, and set by dividing the unnormalised flux (Equation 2) by the unnormalised r-band flux, and then multiplyingF b by the desiredr-band flux, de- termined bym. We discretise the 3D distributionp(t,z,m)in a 3D histogram of"},{"citing_arxiv_id":"2605.13547","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"UNIONS-3500 Weak Lensing: III. 2D Cosmological Constraints in Configuration Space","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T13:55:32+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"UNIONS-3500 weak lensing data yields S_8 = 0.831^{+0.067}_{-0.078} in flat LCDM from 2D cosmic shear, consistent with Planck within 1 sigma.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"same W3 CFHTLenSBPZ(Benítez 2000) catalogue from which the 𝑛(𝑧)wasderived.Wethenadoptthecommonlyemployedmethodof splittingintrinsicalignmentcontributionscomingfromredandblue galaxies (Krause et al. 2016), motivated by the distinction between pressure-supportedandrotationallysupportedgalaxies,respectively. The parametrisation is given by 𝐴IA =𝑓 r 𝐴IA,r +𝑓 b 𝐴IA,b .(30) where𝑓 r indicates the fraction of red galaxies, and𝑓b indicates the fraction of blue galaxies within our sample. For simplicity, we do not introduce any luminosity or redshift dependence, hence𝐴IA is a constant parameter. To separate blue from red galaxies, we choose to assign all galaxies with𝑇𝐵 <1.9as red galaxies and treat the rest as blue. The determination of the𝑇𝐵 index is done through"},{"citing_arxiv_id":"2605.11658","ref_index":8,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Density-Shear Baryon Acoustic Oscillation as a Cosmological Consistency Check","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T07:20:14+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First GI BAO measurement from DES Y3 photometric data yields α = 0.966 ± 0.252, consistent with density BAO α = 0.966 ± 0.037 at 0.86σ detection.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"known tension is the Hubble tension, i.e., the Hubble parameter inferred from the CMB differs from the local SNe measurements by more than 5σ[3]. TheS8 tension is another notable example, in which theS 8 value in- ferred from CMB is higher than the lensing constraints. While some analyses point to settle this tension [4-7], yet it persists in others [8, 9]. Consistency checks across datasets help address these tensions. Baryon Acoustic Oscillations (BAO) are the imprint of the sound horizon feature in the large-scale structure due to the acoustic oscillations in the primordial plasma, and it is generally regarded as a standard ruler in cosmology [10, 11]. This feature provides a powerful cosmological"},{"citing_arxiv_id":"2605.06790","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Machine Learning Techniques for Astrophysics and Cosmology: Photometric Redshifts","primary_cat":"astro-ph.IM","submitted_at":"2026-05-07T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"AI techniques for photometric redshift estimation have converged and are now limited by the size, systematics, and selection effects in spectroscopic training samples rather than by methodology.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"This finding sparked a debate in the community, with proposed solutions ranging from \"new\" physics to observational systematics [27]. Two recent cosmic shear results seem to suggest that the origin of this tension lies in the latter. An improved redshift estimation method and cal- ibration sample was the main change in the KiDS-Legacy cosmic shear analysis [28] that led the collaboration to infer a value ofS 8 =0.815 +0.016 −0.021, with no hint of a tension with the CMB. Similarly, a re-analysis of HSC Y3 data using a new cali- bration of the tomographic redshift distributions via DESI clustering redshifts [29] shifted theS 8 value considerably higher towards Planck cosmology. The most pre- cise such measurement to date is likewise not adding to theS 8 tension: the cosmo-"},{"citing_arxiv_id":"2605.05203","ref_index":128,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Non-conservation and time non-locality of biased tracers","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T17:59:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Non-conserved biased tracers debias more rapidly than conserved tracers, leading to time-dependent suppression of large-scale power.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00821","ref_index":24,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Optimization of Weak Lensing Lightcone Simulations for Higher-Order Statistics in the LSST era","primary_cat":"astro-ph.CO","submitted_at":"2026-05-01T17:57:53+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Uniform discretization in scale factor and 2048^3 particle resolution allow reducing mass shells to ~50 and downsampling high-redshift particles with only 0.1-0.3 sigma impact on higher-order cosmic shear statistics under LSST-like conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00818","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"$4\\times3$ Point Correlation Functions in Galaxy Surveys: Impact of Baryonic Feedback","primary_cat":"astro-ph.CO","submitted_at":"2026-05-01T17:57:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Baryonic feedback affects galaxy-galaxy, galaxy-shear, and shear-shear three-point correlation functions more strongly than two-point functions on small scales, reaching up to 90 percent suppression depending on redshift and model parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Raveri et al., Dark energy survey year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty, Phys. Rev. D105(2022) 023515 [2105.13544]. - 34 - 100 101 102 ϑ [arcmin] 20 40 ϑ × wij(ϑ) [1, 1] 100 101 102 ϑ [arcmin] 10 20 [2, 2] 100 101 102 ϑ [arcmin] 5 10 [3, 3] 100 101 102 ϑ [arcmin] 2.5 5.0 [4, 4] 100 101 102 ϑ [arcmin] 0 2 [5, 5] (a) Galaxy-galaxy 2PCF (w ij(ϑ)). 100 101 102 ϑ [arcmin] 0 1 [1, 1] 100 101 102 ϑ [arcmin] 0.0 2.5 [1, 2] 100 101 102 ϑ [arcmin] 0 5 [1, 3] 100 101 102 ϑ [arcmin] 0 5 [1, 4] 100 101 102 ϑ [arcmin] 0 10 [1, 5] 100 101 102 ϑ [arcmin] 0 1 [2, 2] 100 101 102 ϑ [arcmin] 0.0 2.5 [2, 3] 100 101 102 ϑ [arcmin] 0 5 [2, 4] 100 101 102 ϑ [arcmin] 0 10 [2, 5]"},{"citing_arxiv_id":"2604.28013","ref_index":37,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cosmological intercept tension","primary_cat":"astro-ph.CO","submitted_at":"2026-04-30T15:31:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Tensions in the supernova intercept a_B at z~0.01 in PantheonPlus and z~0.1 in DES-Y5 point to data systematics or inter-survey inconsistencies rather than new physics, aligning H0 measurements and reducing support for dynamical dark energy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A useful way to sharpen this discussion is to distinguish different projections of the Hubble tension. If one attributes the discrepancy to early-Universe physics while keeping the standard late-Universe,theproblemappearsasasound-horizon𝑟 𝑠 tension[4-7]. Thereductionof𝑟 𝑠 tension is achieved at a price of pushing the scalar spectral index closer to the Harrison-Zeldovich scale- invariantspectrumvia𝛿𝑛 𝑠 ∼0.4𝛿𝐻 0/𝐻0 [37](see,e.g.,Refs.[38,39]forasingle-fieldinflationary reconcilementofHarrison-Zeldovichspectrum),andalsoenlargingthematterfluctuation𝑆 8tension, as either speeding up the early-Universe expansion history or advancing the recombination history would all require a larger matter fractionΩ𝑚 (thus a larger𝑆8) to match either galaxy clustering or lensing data [21]."},{"citing_arxiv_id":"2604.25828","ref_index":31,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Fast radio burst dispersion is an unbiased tracer of matter on large scales","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T16:37:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FRB dispersion is an approximately unbiased tracer of matter on linear scales, enabling direct constraints on the baryonic parameter B8 independently of feedback and with statistical power comparable to weak lensing using far fewer objects.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"sures of background FRBs with known redshifts are cross- correlated with foreground galaxy number counts, as first proposed by Madhavacherilet al.[6]. This is the math- ematically simplest statistic, as the fixed galaxy redshift eliminates redshift integrals. It also does not suffer from contamination by clustering of FRB sources and is only weakly sensitive to selection effects [31]. Other statistics share the same principal parameter dependencies. The DM-galaxy angular cross-power spectrum for galaxies in a thin shell at redshiftz g and a DM field from background FRBs is [6] C Dg l = ¯ne(zg) (1 +z g)2 χ2g Pdg(k=l/χ g, zg),(6) wherelis the sky multipole andP dg(k, z) is the diffuse- gas-galaxy power spectrum at spatial wave numberk."},{"citing_arxiv_id":"2604.25373","ref_index":24,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Generalizing the CPL Parametrization through Dark Sector Interaction","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T08:38:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Generalized interacting dark energy models with constant or dynamical couplings yield analytical density expressions but are not preferred over LambdaCDM by Bayesian evidence from DESI, Pantheon+, and CMB data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"with data indicating a mild preference for dynamical DE and a recent crossing of the phantom divide in its equation-of-state parameter. Even so, recent Bayesian analyses [22, 23] continue to support the non-dynamical nature of DE, so the debate continues. For a comprehen- sive review of these and other emerging discrepancies, we refer the reader to [24] and the references therein. Beyond these empirical obstacles, the concordance model is not exempt from serious theoretical issues. The observed value of Λ differs from quantum field theory predictions by roughly 120 orders of magnitude, neces- sitating extreme fine-tuning and giving rise to the long- standing cosmological constant problem [25, 26]."},{"citing_arxiv_id":"2604.17162","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Signatures of Suppressed Matter Clustering revealed by Fast Radio Bursts","primary_cat":"astro-ph.CO","submitted_at":"2026-04-18T22:37:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FRB dispersion measures directly constrain suppression of the matter power spectrum due to feedback at k ~ 0.1-3 h/Mpc, reduce posterior variance by a factor of ~8 at k~1 h/Mpc, and exclude extreme large-scale feedback scenarios at ~2 sigma.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"k∼1hMpc −1 reveals agreement at<1σ-level with BAHAMAS, SIMBA and FLAMINGO (including the fgas −8σvariant), while indicating feedback stronger than IllustrisTNG 45 (1.4σ) and weaker than Illustris (2.6σ) 17 and OWLS-AGN (1.8σ)18. 11 References [1] Chisari, N. E. et al. Modelling baryonic feedback for survey cosmology. The Open Journal of Astrophysics2, 4, DOI: https://dx.doi.org/10.21105/astro.1905.06082 (2019). 1905.06082. [2] Wright, A. H. et al. KiDS-Legacy: Cosmological constraints from cosmic shear with the com- plete Kilo-Degree Survey. Astronomy and Astrophysics703, A158, DOI: https://dx.doi.org/10.1051/ 0004-6361/202554908 (2025). 2503.19441. [3] DES Collaboration et al. Dark Energy Survey Year 6 Results: Cosmological Constraints from Cosmic Shear. arXiv e-printsarXiv:2602."},{"citing_arxiv_id":"2604.12987","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T17:22:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Node-based reconstruction of cosmic expansion prefers stronger deceleration at z≈1.7 than smooth DE EoS parametrizations, isolating z~1.5-2 as a window where the latter may compress localized kinematic features permitted by current data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"from 2019 and 2020 observations of the SPT-3G Main field (2025), arXiv:2506.20707 [astro-ph.CO]. [16] M. Asgariet al.(KiDS), Astron. Astrophys.645, A104 (2021), arXiv:2007.15633 [astro-ph.CO]. [17] E. Di Valentinoet al., Astropart. Phys.131, 102604 (2021), arXiv:2008.11285 [astro-ph.CO]. [18] L. F. Seccoet al.(DES), Phys. Rev. D105, 023515 (2022), arXiv:2105.13544 [astro-ph.CO]. [19] A. H. Wrightet al., Astron. Astrophys.703, A158 (2025), arXiv:2503.19441 [astro-ph.CO]. [20] B. Popovicet al.(DES), The Dark Energy Survey Su- pernova Program: A Reanalysis Of Cosmology Re- sults And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration (2025), arXiv:2511.07517 [astro-ph.CO]. [21] L. Verde, T. Treu, and A."},{"citing_arxiv_id":"2604.08317","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A Dynamical Equilibrium Linking Nanohertz Stochastic Gravitational Wave Background to Cosmic Structure Formation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T14:50:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new generalized Langevin framework for SGWB-matter coupling yields an equilibrium strain spectrum whose cutoff is structurally identified with the LambdaCDM nonlinear mass scale, fitting NANOGrav 15-year data with Bayes factor 48 over the SMBHB baseline.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.03227","ref_index":46,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"UNIONS-3500 Weak Lensing: II. B-mode validation for cosmic shear","primary_cat":"astro-ph.CO","submitted_at":"2026-04-03T17:56:10+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":"2602.03110","ref_index":121,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Evidence for deviation in gravitational light deflection from general relativity at cosmological scales with KiDS-Legacy and CMB lensing","primary_cat":"astro-ph.CO","submitted_at":"2026-02-03T05:11:50+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"KiDS-Legacy weak lensing plus CMB data yields a 3 sigma deviation in light deflection from GR in a Lambda CDM background, with the signal driven by large-scale CMB lensing amplitudes.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"various parametrized models when combined with 3-year weak lensing data from Dark Energy Survey (DESY3) and CMB data (excluding Planck PR3 data 1). The latest weak lensing and CMB data provide new opportunities for testing GR. The Kilo-Degree Survey (KiDS) collaboration has released its final complete weak gravitational lensing measurement, KiDS-Legacy [121, 122]. Covering 1347 deg 2 with nine-band optical/near- infrared deep field imaging, KiDS-Legacy provides ro- bust cosmic shear tomography up toz≤2.0. Notably, through improved redshift calibration and image process- ing techniques, KiDS-Legacy has improved its constrain- ing power on the structure amplitudeS 8 by approxi- mately 32% compared to previous analyses."},{"citing_arxiv_id":"2601.14222","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","primary_cat":"astro-ph.CO","submitted_at":"2026-01-20T18:32:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"[11] T. M. C. Abbottet al.(DES), Phys. Rev. D105, 023520 (2022), arXiv:2105.13549 [astro-ph.CO]. [12] M. Abdul Karimet al.(DESI), Phys. Rev. D112, 083515 (2025), arXiv:2503.14738 [astro-ph.CO]. [13] G. Guet al.(DESI), Dynamical Dark Energy in light of the DESI DR2 Baryonic Acoustic Oscillations Mea- surements (2025), arXiv:2504.06118 [astro-ph.CO]. [14] A. H. Wrightet al., Astron. Astrophys.703, A158 (2025), arXiv:2503.19441 [astro-ph.CO]. [15] D. Broutet al., Astrophys. J.938, 110 (2022), arXiv:2202.04077 [astro-ph.CO]. [16] D. Scolnicet al., Astrophys. J.938, 113 (2022), arXiv:2112.03863 [astro-ph.CO]. [17] T. M. C. Abbottet al.(DES), Astrophys. J. Lett.973, L14 (2024), arXiv:2401.02929 [astro-ph."},{"citing_arxiv_id":"2512.17022","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The contribution from small scales on two-point shear analysis: comparison between power spectrum and correlation function","primary_cat":"astro-ph.CO","submitted_at":"2025-12-18T19:37:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Harmonic-space cosmic shear analysis yields 2-3 times smaller model-choice biases in S8 than real-space analysis when pushing to small scales, with BACCO emulator plus TATT model giving the most consistent constraints between spaces.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.18741","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nonlinear Matter Power Spectrum from relativistic $N$-body Simulations: $\\Lambda_{\\rm s}$CDM versus $\\Lambda$CDM","primary_cat":"astro-ph.CO","submitted_at":"2025-10-21T15:46:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Relativistic N-body simulations of Lambda_s CDM produce a redshift-dependent crest in the matter power spectrum ratio, peaking at 20-25% near the transition and leaving a 15-20% uplift at z=0 on group scales.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":", KiDS-1000: Combined halo-model cosmology constraints from galaxy abundance, galaxy clustering and galaxy-galaxy lensing, Astron. Astrophys. 675, A189 (2023), 2210.03110. [67] T. M. C. Abbottet al.(DES), Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing, Phys. Rev. D105, 023520 (2022), 2105.13549. [68] A. H. Wrightet al., KiDS-Legacy: Cosmological con- straints from cosmic shear with the complete Kilo-Degree Survey (2025), 2503.19441. [69] S. A. Adil, Ö. Akarsu, M. Malekjani, E. Ó. Colgáin, S. Pourojaghi, A. A. Sen, and M. M. Sheikh-Jabbari, S8 increases with effective redshift inΛCDM cosmol- ogy, Mon. Not. Roy. Astron. Soc.528, L20 (2023), 2303."},{"citing_arxiv_id":"2510.14888","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling nonlinear scales for dynamical dark energy cosmologies with COLA","primary_cat":"astro-ph.CO","submitted_at":"2025-10-16T17:07:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"COLA-based hybrid emulator reproduces nonlinear power spectrum boosts in w0wa models to <2% error vs EuclidEmulator2 and produces <0.3σ shifts in LSST-like cosmic shear parameter constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":", KiDS-1000 cosmology: Constraints from density split statistics, Astronomy & Astrophysics669, A69 (2023), arXiv:2208.02171 [astro-ph.CO]. [16] J. L. van den Busch, A. H. Wright, H. Hildebrandt, M. Bil- icki, M. Asgari,et al., KiDS-1000: Cosmic shear with en- hanced redshift calibration, Astronomy & Astrophysics664, A170 (2022), arXiv:2204.02396 [astro-ph.CO]. [17] T.Tröster,M.Asgari,C.Blake,M.Cataneo,C.Heymans,etal., KiDS-1000 Cosmology: Constraints beyond flatΛCDM, As- tronomy & Astrophysics649, A88 (2021), arXiv:2010.16416 [astro-ph.CO]. [18] A.Dvornik,C.Heymans,M.Asgari,C.Mahony,B.Joachimi, et al., KiDS-1000: Combined halo-model cosmology con- straintsfromgalaxyabundance,galaxyclustering,andgalaxy- galaxy lensing, Astronomy &Astrophysics675, A189 (2023),"},{"citing_arxiv_id":"2510.09153","ref_index":110,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation. XCVI. Cosmology Likelihood for Observables in Euclid (CLOE). 3. Inference and Forecasts","primary_cat":"astro-ph.CO","submitted_at":"2025-10-10T08:57:09+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"CLOE pipeline produces forecasts showing Euclid can reach FoM >400 for dark energy w0 and wa by combining primary probes on synthetic data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.07973","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Towards an application of fourth-order shear statistics I. The information content of $\\langle M_\\mathrm{ap}^4 \\rangle $","primary_cat":"astro-ph.CO","submitted_at":"2025-09-09T17:56:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Derives filters for fourth-order aperture statistics, implements a numerical pipeline achieving 2% precision on Gaussian random fields, and forecasts only minimal extra cosmological constraining power when added to second- and third-order aperture statistics in a DES-Y3-like non-tomographic analysis","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.01759","ref_index":95,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resolving the Planck-DESI tension by nonminimally coupled quintessence","primary_cat":"astro-ph.CO","submitted_at":"2025-08-03T14:00:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Non-minimally coupled quintessence resolves the Planck-DESI Ω_m tension at >3σ while the effective equation of state stays above w=-1 and other tensions on neutrino mass and growth rate are relieved.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(overlapping within 1 σ) for our NMCQ model (solid) than the w0waCDM model (dotted), thus largely resolv- ing the Ω m tension. Moreover, the S8 tension [93, 94] is not worsened as the w0waCDM model does; our model reproduces a closer S8 = 0.8201±0.0083 value to the com- pleted Kilo-Degree Survey Legacy (KiDS-Legacy) mea- surement S8 = 0 .815+0.016 −0.021 [95] with ΛCDM model as shown in Fig. 3 from combined Planck+DESI+DESY5. Pseudo crossing behavior. - For our unified fluid of coupled DM- φ components, we can separate out a would-be standard CDM component from the apparent DM component, and then merge the rest into the scalar field as the apparent DE in our model, that is, ∆ρDM = ρDM − ρDM,0a−3 (6) ρDE = ρφ + ∆ρDM, (7)"}],"limit":50,"offset":0}