{"total":28,"items":[{"citing_arxiv_id":"2606.23651","ref_index":37,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2606.19452","ref_index":70,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Validation of the Hybrid Bias Expansion model for the galaxy bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"First systematic validation shows Hybrid Bias Expansion model for galaxy bispectrum remains accurate up to k=0.25 h/Mpc in DESI-like mocks, outperforming tree-level EFT.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17614","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Joint reconstruction of $H(z)$ and $f\\sigma_8(z)$ with physics informed neural networks","primary_cat":"astro-ph.CO","submitted_at":"2026-06-16T07:19:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PINN-based joint reconstruction of H(z) and fσ8(z) coupled through the GR growth equation recovers the input H0 prior exactly, yields fσ8(z) below ΛCDM at all redshifts, and shows Om(z) departure from flat ΛCDM at low z.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12565","ref_index":219,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Galaxy formation in modified gravity -- II. galaxy halo connection and assembly bias","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T18:16:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations in f(R) gravity show that environment density in the HOD model reduces assembly bias effects to 2-3% at z≲0.5 in both ΛCDM and modified gravity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11309","ref_index":195,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dark Energy Survey Year 3 results: optimized $w$CDM simulation-based inference with weak lensing map-level hybrid statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T18:00:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DES Y3 weak lensing analysis with hybrid map-level statistics and simulation-based inference yields S8 = 0.808 ± 0.017, Ωm = 0.325 ± 0.024, and w < -0.766, improving the figure of merit by 60% over prior state-of-the-art.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10679","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Balancing bias, baryons, and scale cuts in LSST 3x2pt analysis","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T10:32:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A minimal bias model yields unbiased LambdaCDM constraints up to k_max=0.7 h/Mpc but biases neutrino mass estimates, while higher-order bias mimics baryonic suppression in LSST 3x2pt analyses using the new MGL pipeline.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27221","ref_index":76,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2605.15078","ref_index":21,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"background","top_context_polarity":"unclear","context_text":"an approximation to the real galaxy distribution, but is a test case of a non-trivial distribution that is not unimodal. The redshift distribution parameters are both chosen to increase with magnitude bin (mk) in order to replicate some of the behaviour seen in the BPZ priors. Explicitly, we take µ1,k =0.20+0.25m k (9) µ2,k =0.8+0.25m k (10) σ 2 1,k =0.05+0.05m k (11) σ 2 2,k =0.18+0.02m k.(12) whenm k = [19,20,21,22,23,24]. To simulate magnitudes and their errors and galaxy weights, we MNRAS000, 1-14 (2026) KV450 cosmology with BHM n(z)5 0.0 0.5 1.0 1.5 2.0 z 0 1 2 3 4 5 6 7 8p(z) 0.0 0.5 1.0 1.5 2.0 z 0 1 2 3 4 5 6 7 8p(z) 0.0 0.5 1.0 1.5 2.0 z 0 1 2 3 4 5 6 7 8p(z) 0.0 0.5 1.0 1.5 2.0 z 0 1 2 3 4 5 6 7 8p(z) 0.0 0.5 1.0 1.5 2.0 z 0 1 2 3 4 5 6 7 8p(z) Redshift Distribution 1"},{"citing_arxiv_id":"2605.13914","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Amplitude-Growth Degeneracy and Implied $A_s$ Diagnostic for Background-Inert Modified Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T09:41:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Any background-inert λ in coincident f(Q) gravity degenerates with σ80 via an As-D0(λ) link, inflating σ80 to unphysical levels and raising As by 20-30% in tension with Planck unless fixed by As priors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05972","ref_index":204,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A statistical look on kinematic planes of satellite galaxies II: The physics behind their early formation in TNG50 MW/M31-like galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T10:18:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic mass collapse along the principal directions of the local cosmic web during the fast assembly phase of host halos.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04176","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Matter Clustering in Astrid: Reduced Baryonic Suppression from Realistic Black Hole Dynamics","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T18:13:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Realistic black hole dynamics in Astrid reduce baryonic suppression of the matter power spectrum at low redshifts compared to repositioning schemes used in other simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01946","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Constraints on Phenomenological Amplitudes of CMB Anisotropy with Multi-Datasets","primary_cat":"astro-ph.CO","submitted_at":"2026-05-03T16:13:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Lensing amplitude A_L deviates from 1 at up to 3.06 sigma in combined datasets while other phenomenological amplitudes remain consistent with Lambda CDM or are poorly constrained.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"0060,S 8 = 0.832±0.013 from Planck [4]. Only the ΛCDM+A L model yields a mild alleviation of theσ 8 tension. In this scenario, we getσ 8 = 0.7958 +0.0073 −0.0068,S 8 ≡σ 8 p Ωm/0.3 = 0.7965 +0.0097 −0.0098 from PDP, and σ8 = 0.7967 +0.0075 −0.0069,S 8 = 0.7959 +0.0096 −0.0097 from PADP, which have 1.53σtension withS 8 = 0.766 +0.020 −0.014 from KiDS- 1000 [41]. Collectively, introducingA new as an additional parameter to the ΛCDM model barely relieves the Hubble tension and theσ 8 tension. Turning to the AIC analysis, we note that in the ΛCDM+A L model ∆AIC≡AIC−AIC ΛCDM =−1.57 and−6.11 for the PDP and PADP datasets, respectively. This indicates that the ΛCDM+A L model is favored by observational data relative to the standard ΛCDM model."},{"citing_arxiv_id":"2605.00818","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Combined halo-model cosmology constraints from galaxy abundance, galaxy clustering, and galaxy-galaxy lensing, A&A675(2023) A189 [2210.03110]. [11] T. Zhang, S. Sugiyama, S. More, R. Mandelbaum, X. Li, R. Dalal et al., Modelling galaxy clustering and tomographic galaxy-galaxy lensing with hsc y3 and sdss using the point-mass correction model and redshift self-calibration, arXiv e-prints (2025) arXiv:2507.01377 [2507.01377]. [12] C. Heymans, T. Tr¨ oster, M. Asgari, C. Blake, H. Hildebrandt, B. Joachimi et al., Kids-1000 cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints, arXiv e-prints (2020) arXiv:2007.15632 [2007.15632]. [13] The Dark Energy Survey Collaboration, Dark energy survey year 3 results: Cosmological constraints from galaxy clustering and weak lensing, Phys."},{"citing_arxiv_id":"2604.20195","ref_index":135,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Photometric Super-Resolution for Improving Galaxy Morphological Measurements using Conditional Generative Adversarial Networks","primary_cat":"astro-ph.IM","submitted_at":"2026-04-22T05:23:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Neo, a cGAN, super-resolves HSC images to HST-like quality and improves galaxy morphological parameter accuracy by factors of 2-10.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18378","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Fourth-order galaxy-galaxy-lensing: Theoretical framework and direct estimation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T15:04:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The authors derive the fourth-order galaxy-galaxy lensing 4PCF and aperture statistics, implement a numerical pipeline and FFT estimator, and detect the connected ⟨N³ M_ap⟩ signal at SNR ~9 in stage IV mock data over 2000 deg².","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.08449","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Coupled Dark Energy and Dark Matter for DESI: An Effective Guide to the Phantom Divide","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T16:45:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Coupled quintessence-dark matter models can produce an apparent phantom-crossing effective equation of state matching DESI preferences if the scalar field begins frozen in the radiation era.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ing and weak lensing,\" Phys. Rev. D98, 043526 (2018), arXiv:1708.01530 [astro-ph.CO]. [11] Shadab Alamet al.(eBOSS), \"Completed SDSS-IV ex- tended Baryon Oscillation Spectroscopic Survey: Cos- mological implications from two decades of spectroscopic surveys at the Apache Point Observatory,\" Phys. Rev. D 103, 083533 (2021), arXiv:2007.08991 [astro-ph.CO]. [12] Catherine Heymanset al., \"KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints,\" Astron. Astrophys.646, A140 (2021), arXiv:2007.15632 [astro-ph.CO]. [13] Dillon Broutet al., \"The Pantheon+ Analysis: Cos- mological Constraints,\" Astrophys. J.938, 110 (2022), arXiv:2202.04077 [astro-ph.CO]. [14] T."},{"citing_arxiv_id":"2603.09278","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraining Neutrino Mass with the Void Weak Lensing Effect","primary_cat":"astro-ph.CO","submitted_at":"2026-03-10T07:03:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations of void-shear cross-correlation demonstrate that void lensing can constrain total neutrino mass to σ(M_ν)=0.096 eV without shape noise and 0.340 eV with Stage-III-like noise.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.01548","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Photometric Redshift PDFs via Neural Network Classification for DESI Legacy Imaging Surveys and Pan-STARRS","primary_cat":"astro-ph.GA","submitted_at":"2026-02-02T02:28:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Neural network classification with CRPS optimization produces calibrated photometric redshift PDFs for DESI Legacy and Pan-STARRS data, achieving σ_NMAD of 0.0153 on LSDR10 and outperforming regression methods.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.18741","ref_index":60,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Effective Field Theory of Large-Scale Structure, JCAP 05, 005, 1909.05271. [58] T. M. C. Abbottet al.(Kilo-Degree Survey, DES), DES Y3 + KiDS-1000: Consistent cosmology combining cos- mic shear surveys, Open J. Astrophys.6, 2305.17173 (2023), 2305.17173. [59] T. Trösteret al., Cosmology from large-scale structure: ConstrainingΛCDM with BOSS, Astron. Astrophys. 633, L10 (2020), 1909.11006. [60] C. Heymanset al., KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clus- tering constraints, Astron. Astrophys.646, A140 (2021), 2007.15632. [61] R. Dalalet al., Hyper Suprime-Cam Year 3 results: Cos- mology from cosmic shear power spectra, Phys. Rev. D 108, 123519 (2023), 2304.00701. [62] S. Chenet al., Not all lensing is low: An analysis of"},{"citing_arxiv_id":"2510.14888","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"ground lensing and intrinsic alignment removal with self- calibration, Astronomy & Astrophysics673, A111 (2023), arXiv:2301.13437 [astro-ph.CO]. [24] C. Hikage, M. Oguri, T. Hamana, S. More, R. Mandelbaum, et al., Cosmology from cosmic shear power spectra with Sub- aruHyperSuprime-Camfirst-yeardata,PublicationsoftheAs- tronomical Society of Japan71, 43 (2019), arXiv:1809.09148 [astro-ph.CO]. [25] T. Hamana, M. Shirasaki, S. Miyazaki, C. Hikage, M. Oguri, et al., Cosmological constraints from cosmic shear two-point correlation functions with HSC survey first-year data, Publi- cations of the Astronomical Society of Japan72, 16 (2020), arXiv:1906.06041 [astro-ph.CO]. [26] H. Aihara, N. Arimoto, R. Armstrong, S. Arnouts, N. A. Bah- call,et al."},{"citing_arxiv_id":"2503.14743","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"Rev. D 98, 043526 (2018), arXiv:1708.01530 [astro-ph.CO]. [11] M. A. Troxel and others (DES), Phys. Rev. D 98, 043528 (2018), arXiv:1708.01538 [astro-ph.CO]. [12] S. Alam and others (eBOSS), Phys. Rev. D 103, 083533 (2021), arXiv:2007.08991 [astro-ph.CO]. [13] C. Heymans and others, Astron. Astrophys. 646, A140 (2021), arXiv:2007.15632 [astro-ph.CO]. [14] T. M. C. Abbott and others (DES), Phys. Rev. D 105, 023520 (2022), arXiv:2105.13549 [astro-ph.CO]. [15] G. Efstathiou, W. J. Sutherland, and S. J. Maddox, Nature 348, 705 (1990). [16] J. Frieman, M. Turner, and D. Huterer, Ann. Rev. As- tron. Astrophys. 46, 385 (2008), arXiv:0803.0982 [astro- ph]. [17] D. H. Weinberg, M. J. Mortonson, D. J. Eisenstein,"},{"citing_arxiv_id":"2411.12022","ref_index":144,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:35+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape clustering yields Ω_m = 0.2962 ± 0.0095 and σ_8 = 0.842 ± 0.034 in flat ΛCDM, tightening to H_0 = 68.40 ± 0.27 km/s/Mpc with CMB and DESY3, while favoring w_0 > -1, w_a < 0 and limiting neutrino mass sum to < 0.071 eV.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"constraints from shear measured in the Hyper Suprime-Cam Year-3 data combined with galaxy clustering from the Baryon Oscillation Spectroscopic Survey (HSC Y3 + BOSS; [143]); constraints from shear measured in the photometric KiDS-1000 survey combined with spec- troscopic galaxy clustering in BOSS and the 2-degree Field Lensing Survey (2dFLenS) (KiDS- 1000+BOSS+2dFLenS; [144]); and the combined shear and clustering 3 × 2-pt analysis from the DESY3 data [102]. The second-to-bottom whisker shows the constraints from the SDSS RSD+BAO analysis [27] that used a full-shape analysis that was substantially different in de- tail to our Full Modeling. We observe an excellent agreement between DESI DR1 (FS+BAO) and the CMB, both of which are slightly higher than the values inferred from the weak lens-"},{"citing_arxiv_id":"2411.07970","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"While this \"low-redshift\" component is not the most critical one for the cosmological goals of MUST, it will be a valu- able dataset that enables many other complementary cosmo- logical probes, such as the multi-tracer clustering to explore the non-linear regime (e.g., [223,224]), the cross-correlations with weak lensing surveys like CSST &Euclidand other multi-wavelength datasets (e.g., [9, 225, 226]), and the spec- troscopic survey of galaxy clusters (e.g., [227, 228]). For now, we assume that MUST will follow the recipes of DESI to select BGS [208], LRG [209], and ELG [210] sam- ples asz<1.6 LSS tracers. Conceptually, we plan to observe BGS and LRG samples as the bright night targets while ob- serving ELG during the gray and dark nights."},{"citing_arxiv_id":"2404.03002","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:51+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First-year DESI BAO data are consistent with flat LambdaCDM and, when combined with CMB, show a 2.5-3.9 sigma preference for evolving dark energy (w0 > -1, wa < 0) that strengthens with certain supernova datasets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":", Constraints on Cosmology from the Cosmic Microwave Background Power Spectrum of the 2500 deg 2 SPT-SZ Survey, Astrophys. J. 782 (2014) 74 [ 1212.6267]. [17] S. Aiola, E. Calabrese, L. Maurin, S. Naess, B.L. Schmitt, M.H. Abitbol et al., The Atacama Cosmology Telescope: DR4 maps and cosmological parameters , J. Cosmology Astropart. Phys. 2020 (2020) 047 [ 2007.07288]. [18] C. Heymans, T. Tr¨ oster, M. Asgari, C. Blake, H. Hildebrandt, B. Joachimi et al., KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints, A&A 646 (2021) A140 [ 2007.15632]. [19] T.M.C. Abbott, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon et al., Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing ,"},{"citing_arxiv_id":"2402.07716","ref_index":67,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"$\\Lambda_{\\rm s}$CDM cosmology from a type-II minimally modified gravity","primary_cat":"astro-ph.CO","submitted_at":"2024-02-12T15:29:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Λ_s VCDM is a predictive model combining Λ_s CDM with VCDM gravity via an auxiliary scalar field and sigmoid-smoothed potentials to enable stable mirror AdS-to-dS transitions with possible transient acceleration.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"tering constraints, Astron. Astrophys. 646, A140 (2021), 2007.15632. [65] R. Dalal et al., Hyper Suprime-Cam Year 3 results: Cos- mology from cosmic shear power spectra, Phys. Rev. D 108, 123519 (2023), 2304.00701. [66] S. Chen et al. , Not all lensing is low: An analysis of DESI×DES using the Lagrangian Effective Theory of LSS (2024), 2407.04795. [67] J. Kim et al. (ACT, DESI), The Atacama Cosmology Telescope DR6 and DESI: Structure formation over cos- mic time with a measurement of the cross-correlation of CMB Lensing and Luminous Red Galaxies (2024), 2407.04606. [68] L. Faga et al. (DES), Dark Energy Survey Year 3 Results: Cosmology from galaxy clustering and galaxy-galaxy lensing in harmonic space (2024), 2406."},{"citing_arxiv_id":"2304.05203","ref_index":75,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters","primary_cat":"astro-ph.CO","submitted_at":"2023-04-11T13:13:14+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"ACT DR6 CMB lensing map gives σ8 = 0.819 ± 0.015 and H0 = 68.3 ± 1.1 km/s/Mpc, consistent with Planck ΛCDM but 1.7-2.1σ higher in S8 than KiDS, DES, and HSC galaxy surveys.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2304.05202","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth","primary_cat":"astro-ph.CO","submitted_at":"2023-04-11T13:13:13+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"ACT DR6 yields a 2.3% precise CMB lensing power spectrum with A_lens = 1.013 ± 0.023 relative to Planck 2018 Lambda CDM, giving S8 = 0.818 ± 0.022 and no evidence for suppressed structure growth.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2105.13549","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing","primary_cat":"astro-ph.CO","submitted_at":"2021-05-28T01:58:58+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DES Y3 3x2pt analysis constrains S8=0.776±0.017 and Ωm=0.339±0.032 in flat ΛCDM, consistent with Planck CMB results at p=0.13-0.48.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"with a spatially flat universe with about 30% matter (visible and dark) and 70% dark energy. However, the physical nature of the dark energy that causes accelerated expansion remains unknown. The simplest and best-known phenomenological model for dark energy is the energy density of the vacuum, incorporated in the field equa- tions of General Relativity by the cosmological-constant term Λ [29]. The resulting Λ Cold Dark Matter ( ΛCDM) model serves as a benchmark for tests with current and future data. Beyond ΛCDM, there exists a rich set of other potential models to explain cosmic acceleration, including evolving scalar fields, modifications to general relativity, and other physically-motivated possibilities. This has spawned an ac- tive research area focused on describing and modeling dark"}],"limit":50,"offset":0}