{"total":20,"items":[{"citing_arxiv_id":"2605.10102","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"From Large Telescopes to the MUltiplexed Survey Telescope (MUST)","primary_cat":"astro-ph.IM","submitted_at":"2026-05-11T07:18:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MUST is a new 6.5 m telescope designed to deliver simultaneous optical spectra for over 20,000 targets across a 5 deg² field, enabling the largest 3D spectroscopic map of the Universe with redshifts for more than 100 million objects over an 8-year survey.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Are there habitable planets and life beyond our Solar System? The answers to these questions, the \"unknown unknowns\" they help uncover during the process, will lead to a new revolution in science. And, during this endeavor, sur- vey telescopes will be at the center of many ambitious scien- tific projects. In particular for cosmology, extensive surveys of galaxies [15,16] and supernovae [17-19] in the large-scale structures of the Universe confirm that the baryonic matter represents only a tiny fraction of the overall matter density and the Universe is accelerating in expansion under the im- petus of dark energy. Suffice it to say that survey telescopes have established themselves as a foundational pillar of mod- ern observational cosmology."},{"citing_arxiv_id":"2604.25373","ref_index":13,"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":"Cosmological parameters, Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [12] A. G. Riesset al., A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team, Astrophys. J. Lett.934, L7 (2022), arXiv:2112.04510 [astro-ph.CO]. [13] E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field (2025), arXiv:2506.20707 [astro-ph.CO]. [14] S. Casertanoet al.(H0DN), The Local Distance Net- work: a community consensus report on the measure- ment of the Hubble constant at 1% precision (2025),"},{"citing_arxiv_id":"2604.23793","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"From Big Bang Nucleosynthesis to Late-Time Acceleration in $f(Q,L_m)$ Gravity","primary_cat":"gr-qc","submitted_at":"2026-04-26T16:35:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The f(Q, L_m) gravity model fits observational data from BBN to late-time acceleration, acting as a viable quintessence-like alternative to the standard LambdaCDM model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"447, 31 (2006), arXiv:astro-ph/0510447. [4] D. N. Spergel et al., \"First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters,\"Astrophys. J. Suppl. Ser.148, 175 (2003), arXiv:astro-ph/0302209. [5] M. Tegmark et al., \"Cosmological parameters from SDSS and WMAP,\"Phys. Rev. D69, 103501 (2004), arXiv:astro- ph/0310723. [6] S. Cole et al., \"The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final dataset and cosmological implica- tions,\"Mon. Not. R. Astron. Soc.362, 505 (2005), arXiv:astro-ph/0501174. [7] D. J. Eisenstein et al., \"Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies,\"Astrophys. J.633, 560 (2005), arXiv:astro-ph/0501171."},{"citing_arxiv_id":"2604.14504","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Forecasting neutrino mass constraints from the Nancy Grace Roman Space Telescope","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T00:37:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Roman Space Telescope forecasts using Hα galaxy mocks yield m_ν < 0.276 eV (68% CL) with Planck priors via EFT of LSS, and m_ν < 0.36 eV via model-independent phenomenological analysis.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"power spectrum, see e.g., [56-61]) In this model, the galaxy power spectrum is given by Pg(k, µ, z) =A(z)[1 +µ 2W(k, z)β(z)] 2T 2 dw(k)kns (5) ×e −(kµσv )2 2 1 +Q(z)k 2 1 +C(z)k+ Q(z) 10 k2 ! , whereA(z) andβ(z) encode amplitude and linear redshift space distortion information, respectively. Non-linearities in the biased field are modeled by a fitting polynomial ink[ 62]. A Gaussian damping and the kernelW(z, k) are introduced phenomenologically to model nonlinear RSD [ 63-65]. As in [ 52, 53, 55, 66] we use a simple expression forW(k, z): W(k, z) = 1 1 + ∆α∆2(k) ,(6) where ∆αis aO(1) free parameter of the theory, and ∆2 = k3P(k) 2π2 is the dimensionless matter power spectrum related to the variance of the matter overdensity field"},{"citing_arxiv_id":"2604.08449","ref_index":7,"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":"Perlmutteret al.(Supernova Cosmology Project), \"Measurements ofΩandΛfrom 42 High Redshift Super- novae,\" Astrophys. J.517, 565-586 (1999), arXiv:astro- ph/9812133. [6] Will J. Percivalet al.(2dFGRS Team), \"Parameter con- straints for flat cosmologies from CMB and 2dFGRS power spectra,\" Mon. Not. Roy. Astron. Soc.337, 1068 (2002), arXiv:astro-ph/0206256. [7] Shaun Coleet al.(2dFGRS), \"The 2dF Galaxy Redshift Survey: Power-spectrum analysis of the final dataset and cosmological implications,\" Mon. Not. Roy. Astron. Soc. 362, 505-534 (2005), arXiv:astro-ph/0501174. [8] N. Aghanimet al.(Planck), \"Planck 2018 results. VI. Cosmological parameters,\" Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys."},{"citing_arxiv_id":"2512.20383","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Spectrum of Cosmological Rips and Their Observational Signatures","primary_cat":"astro-ph.CO","submitted_at":"2025-12-23T14:14:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A unified dark energy model with sigmoid correction generates a spectrum of rip futures that all fit DESI, Pantheon+, and CMB data at the same level as ΛCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.05653","ref_index":70,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Dark Energy Microphysics with kSZ Tomography","primary_cat":"astro-ph.CO","submitted_at":"2025-11-07T19:00:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fisher-matrix forecasts for LSST- and CMB-S4-like surveys show kSZ tomography tightens constraints on dark energy parameters w0 and wa by 15% and 32% while assessing detectability of perturbations for different sound speeds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.21521","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Synergy between CSST and third-generation gravitational-wave detectors: Inferring cosmological parameters using cross-correlation of dark sirens and galaxies","primary_cat":"astro-ph.CO","submitted_at":"2025-10-24T14:43:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Forecasts that cross-correlating 3G GW dark sirens with CSST photometric galaxies yields 1.04% precision on H0 and 2.04% on Omega_m while also constraining GW clustering bias.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[astro-ph.CO]. [3] Y. Mellieret al.(Euclid), Astron. Astrophys.697, A1 (2025), arXiv:2405.13491 [astro-ph.CO]. [4] P. A. Abellet al.(LSST Science, LSST Project), (2009), arXiv:0912.0201 [astro-ph.IM]. [5] Y. Gonget al.(CSST), (2025), arXiv:2507.04618 [astro- ph.IM]. [6] S. Dodelsonet al.(SDSS), Astrophys. J.572, 140 (2001), arXiv:astro-ph/0107421. [7] S. Coleet al.(2dFGRS), Mon. Not. Roy. Astron. Soc. 362, 505 (2005), arXiv:astro-ph/0501174. [8] D. J. Eisensteinet al.(SDSS), Astrophys. J.633, 560 (2005), arXiv:astro-ph/0501171. [9] E. A. Kazinet al.(SDSS), Astrophys. J.710, 1444 (2010), arXiv:0908.2598 [astro-ph.CO]. [10] C. Bonvin and R. Durrer, Phys. Rev. D84, 063505 (2011), arXiv:1105.5280 [astro-ph."},{"citing_arxiv_id":"2509.14322","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the limits of cosmological information from the Lyman-$\\alpha$ forest 2-point correlation functions","primary_cat":"astro-ph.CO","submitted_at":"2025-09-17T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Using idealized synthetic data, knowing the true continuum in Lyα forest auto- and cross-correlations reduces uncertainties on the AP parameter and Ω_m by ~10%, with extension to 240 h^{-1}Mpc scales adding up to ~15% further improvement equivalent to a 40% larger survey area.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.05467","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Combined tracer analysis for DESI 2024 BAO","primary_cat":"astro-ph.CO","submitted_at":"2025-08-07T15:06:22+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Combining LRG and ELG tracers with bias weighting improves BAO constraints by 11% on alpha_iso and 7% on alpha_AP in DESI DR1 data for the 0.8 -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Since the first clear detections of BAO in the Sloan Digital Sky Survey and the Two-Degree Field Galaxy Redshift Survey [7, 8], BAO measurements have played a central role in observational cosmology. The key tech- nical requirement is a large-volume spectroscopic survey with sufficient sampling density, and previous surveys de- signed with BAO measurements as a defining goal include WiggleZ [9], the Baryon Oscillation Spectroscopic Survey (BOSS) [10] of SDSS-III [11], and its extension eBOSS [12] in SDSS-IV [13]. In addition to galaxy and quasar redshifts, BOSS and eBOSS measured BAO in the Ly α forest absorption spectra of z > 2 quasars, an approach first proposed by [14, 15]. Transverse BAO can also be measured in photometric surveys (e."},{"citing_arxiv_id":"2411.12022","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"background","top_context_polarity":"background","context_text":"267 (1982) 465. [5] V. de Lapparent, M.J. Geller and J.P. Huchra, The Mean Density and Two-Point Correlation Function for the CfA Redshift Survey Slices , ApJ 332 (1988) 44. [6] C.M. Baugh and G. Efstathiou, The three-dimensional power spectrum measured from the APM galaxy survey - I. Use of the angular correlation function. , MNRAS 265 (1993) 145. [7] S. Cole, W.J. Percival, J.A. Peacock, P. Norberg, C.M. Baugh, C.S. Frenk et al., The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications, MNRAS 362 (2005) 505 [ astro-ph/0501174]. [8] M. Tegmark, D.J. Eisenstein, M.A. Strauss, D.H. Weinberg, M.R. Blanton, J.A. Frieman et al., Cosmological constraints from the SDSS luminous red galaxies , Phys."},{"citing_arxiv_id":"2411.12021","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:34+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape galaxy clustering constrains Omega_m = 0.296 ± 0.010, H0 = 68.63 ± 0.79 km/s/Mpc, and sigma_8 = 0.841 ± 0.034, consistent with LambdaCDM and Planck.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"dark matter [3] and indicated a matter density below the Einstein-de Sitter prediction [4]. In the 1990s and 2000s, surveys like the 2dF Galaxy Redshift Survey (2dFGRS, [5]) and the Sloan Digital Sky Survey (SDSS, [6]) significantly expanded these datasets in density and volume, enabling crucial validations of the standard model of cosmology, such as the measurement of baryon acoustic oscillations (BAO, [7-9]) and tests of gravity through redshift space distortions (RSD, [10, 11]). The Dark Energy Spectroscopic Instrument (DESI [12-15]) represents the next step in this evolution. DESI is designed to collect spectra for about 40 million galaxies and quasars in the redshift range 0< z <4 thanks to its 5,000 robotic fibre positioners [16] and to the 3.2-degree diameter prime focus corrector [17]."},{"citing_arxiv_id":"2411.07970","ref_index":76,"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":"background","top_context_polarity":"background","context_text":"mological model for redshift-to-distance conversion, has also been shown as a complementary probe of dark energy [75]. Observational programs for measuring the dark energy EoS have been strategically planned to proceed through suc- cessive stages of cosmic surveys, as outlined in the Dark En- ergy Task Force report [15]. Since the first detections of the BAO signal from galaxies atz<0.47 [12, 76], subsequent spectroscopic surveys have extended BAO measurements to galaxies across a wide redshift range (up toz<1.5), as well as QSOs and Lyman-αtracers at even higher redshifts [10]. These efforts have substantially improved the precision ofw measurements. Recently, DESI, a Stage-IV dark energy sur- vey, reported awconsistent withΛCDM with an uncertainty"},{"citing_arxiv_id":"2404.03002","ref_index":50,"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":"The accuracy with which the BAO feature may be measured from a galaxy survey is principally limited by sample variance and Poisson noise in the galaxy clustering measure- ments, necessitating galaxy surveys with effective volume of at least 1 h−3 Gpc3 [43-45].1 The BAO feature was first detected in 2005 by the Sloan Digital Sky Survey (SDSS) [49] and the Anglo-Australian Telescope Two-degree Field Galaxy Redshift Survey [50]. Subsequent measurements, leading to distance determinations accurate to within a few percent, were performed using the SDSS-III Luminous Red Galaxy Sample [51, 52], the WiggleZ Dark En- ergy Survey [53-55] and the 6-degree Field Galaxy Survey [56, 57]. Further extensions of the SDSS yielded more accurate percent-level BAO measurements using the Baryon Oscillation"},{"citing_arxiv_id":"2404.03001","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:50+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI measures BAO from the Lyα forest at z_eff=2.33, reporting H(z) = (239.2 ± 4.8) (147.09 Mpc/rd) km/s/Mpc and DM(z) = (5.84 ± 0.14) (rd/147.09 Mpc) Gpc.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations, arXiv e-prints (2024) arXiv:2404.03002 [ 2404.03002]. [10] D. J. Eisenstein, I. Zehavi, D. W. Hogg, R. Scoccimarro, M. R. Blanton, R. C. Nichol et al., Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies, ApJ 633 (2005) 560 [ astro-ph/0501171]. [11] S. Cole, W. J. Percival, J. A. Peacock, P. Norberg, C. M. Baugh, C. S. Frenk et al., The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications, Mon. Not. Roy. Astron. Soc. 362 (2005) 505 [ astro-ph/0501174]. [12] K. S. Dawson, D. J. Schlegel, C. P. Ahn, S. F. Anderson, 'E. Aubourg, S. Bailey et al."},{"citing_arxiv_id":"2404.03000","ref_index":26,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:49+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI measures BAO scales in six redshift bins with 0.52% combined precision using 5.7 million objects, detecting the signal at up to 9.1 sigma and finding larger scales than Planck LCDM at z<0.8.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"even in the presence of significant observational systematics. This has been demonstrated previously in the literature [19-22], and we explicitly show this for our data as well [23, 24]. The large scale and relatively low amplitude of the BAO feature required the advent of large volume galaxy surveys for it to be detected. The BAO feature was first detected in galaxy clustering by the SDSS [25] and 2dFGRS [26] surveys. The success of these mea- surements prompted the development of the next generation of spectroscopic surveys, most notably the 6dFGS [27], BOSS [28], eBOSS [4] and WiggleZ [29] surveys, that made distance measurements with increasing precision at redshifts 0 < z < 1. The BOSS and eBOSS [30] surveys also demonstrated that the BAO method using the Lyman- α forest, both in the"},{"citing_arxiv_id":"2105.13549","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"(WMAP), Astrophys. J. Suppl. 208, 19 (2013), arXiv:1212.5226 [astro-ph.CO]. [13] N. Aghanim et al. (Planck), Astron. Astrophys. 641, A6 (2020), arXiv:1807.06209 [astro-ph.CO]. [14] S. Aiola et al. (ACT), JCAP12, 047 (2020), arXiv:2007.07288 [astro-ph.CO]. [15] S. Cole et al. (2dFGRS), Mon. Not. Roy. Astron. Soc.362, 505 (2005), arXiv:astro-ph/0501174 [astro-ph]. [16] M. Tegmark et al. (SDSS), Phys. Rev. D 74, 123507 (2006), arXiv:astro-ph/0608632 [astro-ph]. [17] C. Blake et al., Mon. Not. Roy. Astron. Soc. 425, 405 (2012), arXiv:1204.3674 [astro-ph.CO]. [18] E. Aubourg et al., Phys. Rev. D 92, 123516 (2015), arXiv:1411.1074 [astro-ph.CO]. [19] S. Alam et al. (BOSS), Mon. Not. Roy. Astron. Soc.470, 2617 (2017), arXiv:1607."},{"citing_arxiv_id":"1807.06209","ref_index":80,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. VI. Cosmological parameters","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Final Planck CMB data confirms the flat 6-parameter ΛCDM model with Ω_c h² = 0.120 ± 0.001, Ω_b h² = 0.0224 ± 0.0001, n_s = 0.965 ± 0.004, τ = 0.054 ± 0.007, H_0 = 67.4 ± 0.5 km/s/Mpc, and no strong evidence for extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}