{"total":55,"items":[{"citing_arxiv_id":"2606.31324","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological Viability of Exponential Infrared $f(T)$ Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-06-30T08:27:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Exponential IR f(T) gravity Model I alleviates Hubble tension but is disfavoured by combined Planck/ACT/SPT+DESI+Pantheon+ data; Model II is ruled out because background constraints force unphysical shifts in CMB parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"However, despite decades of experimental effort, no evidence for WIMPs has been ∗ mahmoud.hashim@bue.edu.eg † e.divalentino@sheffield.ac.uk ‡ jsaid01@um.edu.mt § waleed.elhanafy@bue.edu.eg arXiv:2606.31324v1 [astro-ph.CO] 30 Jun 2026 2 found, and their allowed parameter space is becoming increasingly constrained by searches at the Large Hadron Collider (LHC) [15] and by direct-detection experiments [16]. At the same time, the physical origin of the dark- energy component responsible for the late-time acceleration of the Universe remains one of the outstanding open questions in cosmology. 2.TheH 0 tension:CMB observations interpreted within the ΛCDM model predictH 0 = 67.19±0.38 km s−1 Mpc−1 [13], in significant (≳5σ) tension with local distance-ladder measurements [17-50]."},{"citing_arxiv_id":"2606.29811","ref_index":57,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Light Neutralino Dark Matter in a Supersymmetric Pati-Salam Framework","primary_cat":"hep-ph","submitted_at":"2026-06-29T05:45:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"In the supersymmetric Pati-Salam framework, light bino-like neutralino dark matter below 110 GeV survives all constraints in bulk and Z-funnel regions for negative mu, with a right-handed stau next-to-lightest particle below 120 GeV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28310","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining primordial oscillations and inflationary particle production with Planck, ACT DR6, and DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T17:54:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Using combined CMB and LSS observations, the analysis sets 95% CL upper limits on oscillatory amplitudes at approximately 2% of A_s and a MAP value of 0.034 for the particle production coupling constant, finding no statistical preference for the extended models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26576","ref_index":203,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detectors for CLASS-W2: The second 90 GHz telescope of the Cosmology Large Angular Scale Surveyor","primary_cat":"astro-ph.IM","submitted_at":"2026-06-25T03:52:30+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A new 296-detector 90 GHz TES bolometer array for CLASS achieves uniform properties, 16 μK√s NET, 0.37 optical efficiency, and a 41% mapping speed boost after addressing blue-leak radiation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Scott, E. P. S. Shellard, M. Shiraishi, C. Sirignano, G. Sirri, L. D. 28 Spencer, R. Sunyaev, A. S. Suur-Uski, J. A. Tauber, D. Tavagnacco, M. Tenti, L. Terenzi, L. Toffolatti, M. Tomasi, T. Trombetti, J. Valiviita, B. Van Tent, L. Vibert, P. Vielva, F. Villa, N. Vittorio, B. D. Wandelt, I. K. Wehus, M. White, S. D. M. White, A. Zacchei, and A. Zonca, \"Planck 2018 results. I. Overview and the cosmological legacy of Planck,\"Astronomy & As- trophysics641, p. A1, Sept. 2020. 3 G. Hinshaw, D. Larson, E. Komatsu, D. N. Spergel, C. L. Bennett, J. Dunkley, M. R. Nolta, M. Halpern, R. S. Hill, N. Odegard, L. Page, K. M. Smith, J. L. Weiland, B. Gold, N. Jarosik, A. Kogut, M. Limon, S. S. Meyer, G. S. Tucker, E. Wollack, and E."},{"citing_arxiv_id":"2606.25158","ref_index":159,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T20:45:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13527","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Machine Learning Does It and Does It Better: Unearthing Primordial Dark-Matter Velocities from the Matter Power Spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-06-11T16:17:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A 1D convolutional neural network reconstructs the dark-matter phase-space distribution from the matter power spectrum with greater accuracy and broader applicability than an earlier empirical formula.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12549","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tachyonic Encore: A universal shift of inflationary observables","primary_cat":"hep-th","submitted_at":"2026-06-10T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A light axion spectator induces post-inflation tachyonic phases that produce a nearly scale-invariant boost to the curvature power spectrum and alter key inflationary observables in a largely potential-independent manner.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11368","ref_index":5,"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":"2606.10597","ref_index":66,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Synergy between the gravitational potential decay rate and other structure growth probes in testing gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T09:01:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Tomographic DR data added to Σ8 + fσ8 tightens phenomenological MG parameters (μ0, Σ0, η0) and EFT α coefficients by factors of 1.5–2.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10020","ref_index":51,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Manticore Project II: Bayesian digital twins of cosmic structure across the SDSS and BOSS volumes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:07:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Manticore-Deep uses tiled Bayesian field-level inference on SDSS and BOSS data to produce posterior ensembles of 3D cosmic fields that are consistent with LCDM and validated by 7.4σ CMB lensing and 3.5σ kSZ detections.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09650","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Pantheon+ supernovae corrected for progenitor age indicate the universe is decelerating","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T15:41:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Progenitor age corrections applied to Pantheon+ data shift the monopole q0 to positive values (deceleration) while the local dipole remains unchanged.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09945","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Geometric Matching of Local Static Regions in Cosmological Spacetimes with an Evolving Lapse","primary_cat":"gr-qc","submitted_at":"2026-06-08T06:47:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Embedding a static Schwarzschild interior into a GCT-FLRW exterior via Israel junction conditions produces a geometric consistency condition that coincides with the GCT background equations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06969","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lyman-$\\alpha$ forest constraints on pure and mixed fuzzy dark matter","primary_cat":"astro-ph.CO","submitted_at":"2026-06-05T06:57:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Lyman-alpha forest data yield m_FDM > 1.9e-21 eV (95% CL) for pure FDM and f_FDM upper limits of 0.07-0.65 for mixed FDM at log10(m_FDM/eV) = -23 to -21.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05166","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Compressed Gaussian likelihood for the Planck low-$\\ell$ data","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T17:59:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A compressed Gaussian likelihood for Planck low-ℓ data is built from SRoll2 via offset log-normal functions for Fisher compatibility and validated against the original via MCMC.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00176","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eigenvalue formulation of Stochastic Inflation and application to large perturbation generating inflationary features","primary_cat":"astro-ph.CO","submitted_at":"2026-05-29T13:57:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new eigenvalue method is introduced to compute the PDF of stochastic e-folds in inflation, recovering a known flat-potential result and analyzing constant-drift cases in narrow and broad well limits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27520","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Ellis and Baldwin test of the Cosmic Dipole: Exploring the impact of multiple flux density cuts","primary_cat":"astro-ph.CO","submitted_at":"2026-05-26T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A multi-bin simultaneous dipole fitting method yields higher Bayes factors than single flux-cut approaches for non-power-law luminosity functions in cosmic dipole measurements.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27301","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effective Phantom Dark Energy: What Cosmological Reconstruction Does and Does Not Imply","primary_cat":"astro-ph.CO","submitted_at":"2026-05-26T17:11:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Effective phantom dark energy is a background-level reconstruction that does not imply fundamental pathologies such as ghost instabilities or null energy condition violation by the underlying stress tensor.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cambridge Uni- versity Press, Jan. 2015.isbn: 978-1-107-45398-2. [6] G. Hinshaw et al. \"Nine YearWilkinson Microwave Anisotropy Probe(WMAP) Observa- tions: Cosmological Parameter Results\". In:The Astrophysical Journal Supplement Series 208.2 (2013), p. 19.issn: 1538-4365.doi:10.1088/0067- 0049/208/2/19.url:http: //dx.doi.org/10.1088/0067-0049/208/2/19. [7] N. Aghanim et al. \"Planck 2018 results. I. Overview and the cosmological legacy of Planck\". In:Astron. Astrophys.641 (2020), A1.doi:10 . 1051 / 0004 - 6361 / 201833880. arXiv: 1807.06205 [astro-ph.CO]. [8] T. Louis et al. \"The Atacama Cosmology Telescope: DR6 power spectra, likelihoods and ΛCDM parameters\". In:JCAP11 (2025), p. 062.doi:10.1088/1475-7516/2025/11/062."},{"citing_arxiv_id":"2605.19476","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Prospect of Measuring the Cosmic Dipole by Strongly Lensed Gravitational Waves Associated with Galaxy Surveys","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T07:28:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Simulations forecast that 10 years of Einstein Telescope and Cosmic Explorer data could detect the cosmic dipole magnitude using strongly lensed GW events, with tighter bounds from combining double, triple, and quadruple lensed systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16587","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"3d QFT IR divergences as UV divergences in 4d Holographic Cosmology","primary_cat":"hep-th","submitted_at":"2026-05-15T19:45:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In a 3d toy model for holographic cosmology, a mass term preserving generalized conformal structure permits 2-loop computations that indicate possible IR finiteness beyond perturbation theory, corresponding to UV finiteness without singularities in the 4d dual.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15947","ref_index":40,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dipoles for everyone: the pseudo-$C_\\ell$ approach to directional stacking","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T13:30:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Directional stacking signals are reconstructed without information loss as cross-power spectra between the target field and the E/B modes of the spin field weighted by galaxy density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16426","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Expected redshift drift for tilted observers","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T15:49:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Redshift drift for tilted observers consists of an FLRW background term plus directional corrections from peculiar expansion, projected shear, and acceleration along the line of sight.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12499","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Measuring cosmic bulk flow with kinetic Sunyaev-Zel'dovich velocity reconstruction","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T17:59:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Kinetic Sunyaev-Zel'dovich reconstruction from WISExSuperCOSMOS and unWISE galaxies with Planck data yields tight upper limits on bulk velocities consistent with LambdaCDM out to 2000 h^{-1} Mpc while showing tension with a quasar dipole interpretation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Kogut, E. Komatsu, D. Larson, M. Limon, S. S. Meyer, M. R. Nolta, N. Odegard, L. Page, K. M. Smith, D. N. Spergel, G. S. Tucker, J. L. Weiland, E. Wollack, and E. L. Wright, Seven-year wilkinson microwave anisotropy probe ( wmap ) observations: Sky maps, systematic er- rors, and basic results, The Astrophysical Journal Sup- plement Series192, 14 (2011). [41] N. Battaglia, The tau of galaxy clusters, Journal of Cos- mology and Astroparticle Physics2016(08), 058-058. [42] S. Flender, D. Nagai, and M. McDonald, Constraints on the Optical Depth of Galaxy Groups and Clusters, Astrophys. J.837, 124 (2017), arXiv:1610.08029 [astro- ph.CO]. [43] M. S. Madhavacheril, N. Battaglia, K. M. Smith, and J. L. Sievers, Cosmology with the kinematic sunyaev-"},{"citing_arxiv_id":"2605.10928","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Mitigating residual foregrounds and systematic errors in SKA1-Low AA* EoR observations via Bayesian Gaussian Process Regression","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T17:57:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian GPR recovers the 21cm signal within 2σ credible intervals for most k-modes (0.06 to 1.0 h/Mpc) in SKA1-Low simulations that include realistic residual foregrounds and systematics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In Section 4, we outline the detailed procedure for subtracting residual foregrounds using ML-GPR. In Section 5, we compare the performances of different Bayesian GPR models for extracting the 21cm signal from SKA-Low observations. Finally, in Section 6, we summarize the key findings of this study. In this study, we used theΛCDM cosmology with the Planck 2018 parameter set [42]: Ω𝑀 =0.31,Ω Λ =0.68, 𝜎 8 =0.811, 𝐻 0 =67.36km s −1 Mpc−1. 2 Simulations Wegeneratemockradiointerferometricobservationsusingtheend-to-end21cmE2E 1pipeline [25, 27, 28, 43], which is built on theOSKARsimulation software [44].OSKARuses the Radio Interferometer Measurement Equation(RIME) [45] to generate full-Stokes visibility data. This pipeline includes realistic sky models, telescope configurations, and the time-"},{"citing_arxiv_id":"2605.08907","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The Status of Gravitational Vector Perturbations with Recent CMB Data","primary_cat":"astro-ph.CO","submitted_at":"2026-05-09T12:05:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Recent CMB datasets tighten 95% CL upper bounds on vector-mode amplitude r_v to 1.3e-4 (neutrino isocurvature), 6.8 (octupole), and 4.2 (sourced) at k=0.05 Mpc^-1, with no significant detection.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":", The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models , arXiv:2503.14454. [28] ACT Collaboration, Sigurd Naess et al., The Atacama Cosmology Telescope: DR6 Maps , arXiv:2503.14451. [29] Planck Collaboration, N. Aghanim et al., Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys. 641 (2020) A6, [ arXiv:1807.06209]. [30] Planck Collaboration, N. Aghanim et al., Planck 2018 results. I. Overview and the cosmological legacy of Planck, Astron. Astrophys. 641 (2020) A1, [ arXiv:1807.06205]. [31] SPT Collaboration, J. T. Sayre et al., Measurements of B-mode Polarization of the Cosmic Microwave Background from 500 Square Degrees of SPTpol Data , Phys. Rev. D 101 (2020), no."},{"citing_arxiv_id":"2605.04983","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Capturing statistical isotropy violation with rotational averages","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T14:35:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Rotational averages of the angular correlation function isolate non-statistical isotropy components in the CMB sky as a real-space complement to BipoSH coefficients.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The bottom panel illustrates the fractional difference between the real and harmonic space computations. The real space computation involves aver- aging over 107 rotations. Note that the fractional different increase for higher values ofL. [3] Dominik J Schwarz et al. \"CMB anomalies after Planck\". In:Classical and Quantum Gravity33.18 (Aug. 2016), p. 184001.doi:10.1088/0264-9381/33/18/184001. [4] N. Aghanim et al. \"Planck 2018 results. I. Overview and the cosmological legacy of Planck\". In:Astron. Astrophys.641 (2020), A1.doi:10 . 1051 / 0004 - 6361 / 201833880. arXiv: 1807.06205 [astro-ph.CO]. [5] Simon Prunet et al. \"Constraints on mode couplings and modulation of the CMB with WMAP data\". In:Phys. Rev. D71 (2005), p. 083508.doi:10.1103/PhysRevD."},{"citing_arxiv_id":"2604.26015","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Kinematic Lensing Ratio: Reviving Weak Lensing Cosmography as a Geometric Dark Energy Probe","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T18:00:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"KiLeR combines shear ratios with kinematic intrinsic shapes to mitigate first-order lensing systematics and forecasts a 192% improvement in dark energy constraints from the Roman telescope.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ments on systematic and statistical errors and discuss the pathways towards KiLeR observation. WEAK LENSING COSMOGRAPHY The nature of cosmic acceleration remains one of the most profound mysteries in fundamental physics (for a re- view, see [1]). While the standard ΛCDM model, which interprets the acceleration as driven by Einstein's cosmo- logical constant (Λ), has been remarkably successful in the era of the Planck satellite [2, 3], recent Dark Energy Spectroscopic Instrument (DESI) analysis [4-6] reported ∼3−4σevidence of evolving dark energy. This potential discovery marks a pivotal shift in community focus from constraining the density parameter ΩDE to characterizing the time-evolution of the equation of state,w(z). As Baryon Acoustic Oscillation (BAO) measurements at low redshifts (z <1) approach the cosmic variance un-"},{"citing_arxiv_id":"2604.22462","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Machine Learning for Multi-messenger Probes of New Physics and Cosmology: A Review and Perspective","primary_cat":"hep-ph","submitted_at":"2026-04-24T11:29:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A review summarizing machine learning methods for multi-messenger probes of dark matter and new physics, with a proposed plan for future integrated analyses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"direct GW detection, which was finally attained only few years ago, represents an unprecedented possibility to unveil the micro-physics of DM, providing through current and forthcoming experiments a sizeable amount of information that can be deployed to solve at least some of the current shortcomings. At the same time, data on cosmic rays spectra that will arise from very sensitive experiments like LHAASO [18, 19] will enable to explore energy ranges from 100 GeV to 100 PeV, thus providing further unprecedented possibilities to test these models. We will then discuss here the possibility to carry out multi-messenger numerical analyses of DM candidates that are both either minimal extensions of the Standard Model (SM) of particle physics or arise as more convoluted"},{"citing_arxiv_id":"2604.18007","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"In-depth analysis of the clustering of dark matter particles around primordial black holes. Part III: CMB constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T09:30:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Since we are considering self-annihilating DM, the huge densities accumulated in spikes can- not remain unaffected by self-annihilation, and the latter actually regulates the amount of DM right around the BH. Density cores arise from this process, which we try to characterize below. A crude way to describe this process is to consider a simple evolution equation assuming circular orbits [45, 46]: dnχ(r, t) dt =−2× δann⟨σannv⟩ 2 n2 χ(r, t) =− nχ(r, t) tann(nχ) ,(2.15) whereδ ann = 1 (1/2) for Majorana (Dirac) particles, and the first factor of 2 accounts for the disappearance of a pair of particles in an annihilation process. The characteristic WIMP annihilation time is given by: tann ≡ \u001a\u0012 nχ = ρχ mχ \u0013 ⟨σannv⟩ \u001b−1 ,(2.16) wherem χ is the WIMP mass,n χ its number density,ρ χ its corresponding mass density, and"},{"citing_arxiv_id":"2604.14088","ref_index":89,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"BROOM: a python package for model-independent analysis of microwave astronomical data","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T17:04:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"BROOM is a Python package that applies ILC and GILC techniques for model-independent separation of CMB, SZ, and foreground signals in microwave data along with diagnostic and simulation utilities.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"We now proceed to present the results of a validation run of theBROOMpackage in the following section. 4 Validation and results In this section, we present the results of a validation run covering most of the functional- ities of theBROOMpackage. The analysis is divided into two parts: the first one focuses on full-sky observations, representative of satellite CMB experiments (e.g. WMAP [23, 88], Planck[31, 89], LiteBIRD [90], PICO [91, 92]), while the second targets partial-sky measure- ments characteristic of ground-based experiments (e.g. POLARBEAR [93, 94], ACT [95, 96], SPT [3, 97], BICEP/Keck [16, 98], SO [14, 99]). For both cases, we run the complete analysis pipeline provided by the package, including the generation of tailored simulations, the appli-"},{"citing_arxiv_id":"2604.12587","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Impact of the SNe Ia Magnitude Transition at 20 Mpc on Cosmological Parameter Estimation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T11:10:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A 0.19 mag step in supernova absolute magnitude at 20 Mpc improves data fit and increases the Hubble constant by 2% while leaving matter density and dark energy parameters stable.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Guide,\" (2019), arXiv:1908.03663 [astro-ph.CO]. [16] Adam G. Riess, Stefano Casertano, Wenlong Yuan, Lu- cas M. Macri, and Dan Scolnic, \"Large Magellanic Cloud Cepheid Standards Provide a 1% Foundation for the De- termination of the Hubble Constant and Stronger Evi- dence for Physics beyond ΛCDM,\" Astrophys. J.876, 85 (2019), arXiv:1903.07603 [astro-ph.CO]. [17] Dan Scolnicet al., \"The Pantheon+ Analysis: The Full Data Set and Light-curve Release,\" Astrophys. J.938, 113 (2022), arXiv:2112.03863 [astro-ph.CO]. [18] Anthony Carret al., \"The pantheon+ analysis: Improv- ing the redshifts and peculiar velocities of type ia su- pernovae used in cosmological analyses,\" Publications of the Astronomical Society of Australia39(2022),"},{"citing_arxiv_id":"2604.08530","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Disentangling cosmic distance tensions with early and late dark energy","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T17:58:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"those from other observables, small but statistically sig- nificant discrepancies have begun to arise in recent years, the most significant of these being the Hubble tension. Combining the most precise CMB probes results in a best-fit value under ΛCDM of the current expansion rate H0 = 67.24±0.35 [5], while the Local Distance Network (H0DN) collaboration reports a direct measurement of H0 = 73.50±0.81 [6], largely but not exclusively based on the SH0ES Cepheid-supernova Ia local distance lad- der [7, 8]. Here and throughout, the units ofH 0 values are implicitly km s−1 Mpc−1. Taken at face value, this is a 7.1σdiscrepancy, with a vanishingly small associated probability of arising from statistical fluctuations alone. The CCHP group, using a different calibration of the"},{"citing_arxiv_id":"2603.23846","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The read-out electronics for the FLASH experiment","primary_cat":"physics.ins-det","submitted_at":"2026-03-25T02:05:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"FLASH's read-out system uses MSAs as low-noise amplifiers and SDR techniques to capture and process ultra-weak signals from dark matter or high-frequency gravitational waves in the 117-360 MHz range.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.01507","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Anisotropic matter and nonlinear electromagnetics black holes","primary_cat":"gr-qc","submitted_at":"2026-03-02T06:33:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Establishes a parameter mapping from anisotropic matter black holes to nonlinear electrodynamics black holes, recovering known solutions like dark matter and scalar hair cases and extending to rotating extremal limits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.11936","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Dynamical Dark Energy with Late-Time Data: Evidence, Tensions, and the Limits of the $w_0w_a$CDM Framework","primary_cat":"astro-ph.CO","submitted_at":"2026-02-12T13:35:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Evidence for dynamical dark energy in the w0waCDM framework is strongly dataset-dependent, driven by mismatches in low-redshift BAO distance ratios that produce divergent expansion histories and inconsistent Hubble tension relief.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"and on internal consistency among late-time distance probes. We combine CMB anisotropies and lensing with: (i) standard three-dimensional BAO distances from DESI DR2 [6] and from the completed SDSS-IV (BOSS+eBOSS) BAO consensus [5] compilation, (ii) an angular/transverse BAO compilation (BAOtr) [207], and (iii) the Cepheid-calibrated PantheonPlus SN Ia likeli- hood (PP&SH0ES) [7, 8, 24]. Beyond constraints in the (w0, wa)plane, we reconstruct the implied background history via the conformal Hubble rateH(z)/(1 +z)and thedecelerationparameterq(z)anddiscusstheirpresent- day values,H 0 andq 0, and we trackrd and the combi- nationr dH0 to diagnose whether shifts inH0 arise pri- marily from late-time expansion freedom or from changes"},{"citing_arxiv_id":"2602.11093","ref_index":187,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","primary_cat":"astro-ph.CO","submitted_at":"2026-02-11T18:01:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Galaxy cluster observations yield two preferred directions with cosmic anisotropy amplitude of about 5.3 times 10 to the minus 4 at roughly 1 sigma overall significance, though higher in the XMM-Newton subsample.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Deng and H. Wei, Testing the cosmic anisotropy with supernovae data: Hemisphere comparison and dipole fitting, Phys. Rev. D 97 (2018) 123515 [ 1804.03087]. [186] Planck Collaboration, R. Adam, P.A.R. Ade, N. Aghanim, Y. Akrami, M.I.R. Alves et al., Planck 2015 results. I. Overview of products and scientific results , A&A 594 (2016) A1 [1502.01582]. [187] Planck Collaboration, N. Aghanim, Y. Akrami, F. Arroja, M. Ashdown, J. Aumont et al., Planck 2018 results. I. Overview and the cosmological legacy of Planck , A&A 641 (2020) A1 [1807.06205]. [188] S.J. Turnbull, M.J. Hudson, H.A. Feldman, M. Hicken, R.P. Kirshner and R. Watkins, Cosmic flows in the nearby universe from Type Ia supernovae , MNRAS 420 (2012) 447 [ 1111."},{"citing_arxiv_id":"2602.06027","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"ACT DR6+Planck impact on inflation with non-zero vacuum expectation value and the post-inflationary behavior","primary_cat":"astro-ph.CO","submitted_at":"2026-02-05T18:57:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Updated constraints on non-zero VEV parameter M from ACT+Planck data, plus lattice simulations showing oscillon formation and reheating implications.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.14222","ref_index":3,"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":"h≡ H0 100 km−1 s Mpc (dimensionless Hubble constant) and Ω m0 usingCC+BAO+SN+SH0ES+CMBas the dataset combination. [1] C. L. Bennettet al.(WMAP), Astrophys. J. Suppl.208, 20 (2013), arXiv:1212.5225 [astro-ph.CO]. [2] N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [3] N. Aghanimet al.(Planck), Astron. Astrophys.641, A1 (2020), arXiv:1807.06205 [astro-ph.CO]. [4] S. Aiolaet al.(ACT), JCAP12, 047, arXiv:2007.07288 [astro-ph.CO]. [5] T. Louiset al.(Atacama Cosmology Telescope), JCAP 11, 062, arXiv:2503.14452 [astro-ph.CO]. [6] E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmology"},{"citing_arxiv_id":"2601.00790","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Dimension Right-handed Neutrinos Confronted with Long-Baseline Oscillation Experiments","primary_cat":"hep-ph","submitted_at":"2026-01-02T18:48:58+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":"2512.17865","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Constraining primordial non-Gaussianity from DESI DR1 quasars and Planck PR4 CMB Lensing","primary_cat":"astro-ph.CO","submitted_at":"2025-12-19T18:14:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cross-correlation of DESI DR1 quasars with Planck PR4 CMB lensing constrains local f_NL to 2^{+28}_{-34} (p=1.6) or 6^{+20}_{-24} (p=1.0), tightening previous limits by 35%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.02526","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Updates on dipolar anisotropy in local measurements of the Hubble constant from Cosmicflows-4","primary_cat":"astro-ph.CO","submitted_at":"2025-12-02T08:42:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Local Hubble constant anisotropy in Cosmicflows-4 data is primarily attributed to peculiar velocities and survey structure rather than cosmic-scale isotropy violation, with limited implications for the Hubble tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.22641","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Non-Gaussianity in SMICA","primary_cat":"astro-ph.CO","submitted_at":"2025-11-27T17:21:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New SMICA formalism and binned bispectrum estimator jointly recover power spectra, spectral parameters, foreground 3-point correlators, and primordial non-Gaussianity constraints from multi-frequency polarization maps tested on LiteBIRD simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.25886","ref_index":53,"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":"2509.00139","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Deep Learning for CMB Foreground Removal and Beam Deconvolution: A U-Net GAN Approach","primary_cat":"astro-ph.IM","submitted_at":"2025-08-29T17:08:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A U-Net GAN reconstructs CMB T and E maps from Planck-like simulations with foregrounds and systematics, achieving under 1% error outside the Galactic region and demonstrating first-time correction for non-circular beams and asymmetric scans.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.08833","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmic filaments confirm unexplained CMB temperature decrements in two independent redshift ranges","primary_cat":"astro-ph.CO","submitted_at":"2025-06-10T14:20:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The paper detects CMB temperature decrements toward the spines of massive cosmic filaments in two independent nearby redshift ranges using 3D luminosity-density profiles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.22066","ref_index":67,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmic Strings as Dynamical Dark Energy: Novel Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-05-28T07:45:53+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Cosmic string networks are constrained to less than ~1% of the energy density using CMB+BAO+SN data, with some models preferring mildly negative densities but no Bayesian evidence favoring them over LambdaCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.11553","ref_index":107,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Holographic entanglement entropy and complexity for the cosmological braneworld model","primary_cat":"hep-th","submitted_at":"2025-05-15T15:59:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Time-dependent holographic entanglement entropy and complexity are computed perturbatively for braneworld FLRW universes with radiation, matter, and exotic matter by using time-dependent brane positions in black brane bulk geometries.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.12521","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lectures on the Bondi--Metzner--Sachs group and related topics in infrared physics","primary_cat":"gr-qc","submitted_at":"2025-04-16T22:47:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Lecture notes that build the BMS group from prerequisites to applications in soft theorems, memory effects, and new material on asymptotic conformal Killing horizons.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"which is proven on Appendix B. Hence, the group of confomorphisms on the two-sphere is just the restricted Lorentz group! It can also be shown that the group of isometries on the two-sphere is SO(3), as one would expect. This is done by proving the matrices representing the Möbius transformations are now unitary , L†L = 1. As a consequence, they now live in the group SU(2) of 2 × 2 unitary matrices. Up to sign, we get SU(2)/Z2 ∼= SO(3) through arguments analogous to those of Appendix B. 3.5 Case Study: Isometries on Minkowski Spacetime It is instructive to consider as a second case study the isometries in Minkowski spacetime. We should, of course, recover the Poincaré transformations. We work in n-dimensional Minkowski spacetime, for"},{"citing_arxiv_id":"2503.14743","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Extended Dark Energy analysis using DESI DR2 BAO measurements","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:17+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"(which are also present in the PantheonPlus sam- ple) spanning 0 .025 < z < 0.1. • Cosmic microwave background (CMB): We include temperature and polarization measurements of the CMB from the Planck satellite [72]. In par- ticular, we use the high- ℓ TTTEEE likelihood (planck NPIPE highl CamSpec.TTTEEE), together with low- ℓ TT ( planck 2018 lowl.TT) and low- ℓ EE ( planck 2018 lowl.EE) [73, 74], as imple- mented in Cobaya [75]. Additionally, we combine temperature and polarization anisotropies with CMB lensing measurements from the combination of NPIPE PR4 from Planck [76, 77] and the Ata- cama Cosmology Telescope (ACT) DR6 [78, 79]. • Compressed CMB: We use the Gaussian correlated prior over ωb ≡ Ωbh2, ωbc ≡ Ωbh2+Ω ch2 and θ∗ as defined in [47]."},{"citing_arxiv_id":"2503.14738","ref_index":104,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:12+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR2 BAO data exhibits 2.3 sigma tension with CMB in Lambda-CDM but prefers evolving dark energy (w0 > -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"106]) and the South Pole Telescope (SPT; [107]). When using the full power of the CMB information, our baseline analysis makes use of the temperature (T T), polarization ( EE) and cross ( T E) power spectra from Planck, specifically using the simall, Commander (for ℓ < 30) and CamSpec (for ℓ ≥ 30) likelihoods, plus the combination of Planck and ACT DR6 CMB lensing from [104].13 CamSpec [108, 109] is a new likelihood built on the latest NPIPE PR4 data release from the Planck col- laboration, which replaces the original Plik likelihood based on the older PR3 release and includes some im- portant differences in methodology. Another set of like- lihoods based on PR4, known as LoLLiPoP (for low ℓ) and HiLLiPoP (for high ℓ) have also been independently"},{"citing_arxiv_id":"2411.07970","ref_index":276,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys","primary_cat":"astro-ph.CO","submitted_at":"2024-11-12T17:51:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MUST is a planned 6.5m Stage-V spectroscopic survey telescope targeting 100M+ galaxies and quasars to z~5.5 for large-scale structure cosmology studies.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"cally, we focus on the DESI galaxy samples, i.e., BGS, LRG, and ELG. 14) Marginalized means of parameters from thePliklikelihood, see Table 1 of [4]. Zhao, et al. Sci. China-Phys. Mech. Astron.January (2023) V ol. 66 No. 1000000-24 To fully assess the constraining power of next-generation cosmological data, we incorporate external CMB priors from Planck [276] and Simons Observatory (SO; [45]) into our Fisher forecasts, following the methodology in [16]. Addi- tionally, we perform Bayesian cosmological parameter infer- ences using Markov-Chain Monte-Carlo (MCMC) methods without these CMB priors, and directly compare our forecasts to constraints derived from the existing Planck and Atacama Cosmology Telescope (ACT; [277]) CMB data, as well as the"}],"limit":50,"offset":0}