{"total":21,"items":[{"citing_arxiv_id":"2607.06147","ref_index":93,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Imprint of swampland-inspired coupled early dark energy","primary_cat":"astro-ph.CO","submitted_at":"2026-07-07T11:15:39+00:00","verdict":"CONDITIONAL","verdict_confidence":"UNKNOWN","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A swampland-inspired DM-EDE coupling is tested against DESI DR2 BAO data, showing the EDE potential construction affects late-time dark energy constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.01226","ref_index":78,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T17:57:32+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":",The waning of the WIMP? A review of models, searches, and constraints,Eur. Phys. J. C78(2018) 203 [1703.07364]. [76] M. Schumann,Direct Detection of WIMP Dark Matter: Concepts and Status,J. Phys. G46 (2019) 103003 [1903.03026]. [77] A.A. Starobinsky,Spectrum of relict gravitational radiation and the early state of the universe, JETP Lett.30(1979) 682. [78] V.A. Rubakov, M.V. Sazhin and A.V. Veryaskin,Graviton Creation in the Inflationary Universe and the Grand Unification Scale,Phys. Lett. B115(1982) 189. [79] R. Fabbri and M.d. Pollock,The Effect of Primordially Produced Gravitons upon the Anisotropy of the Cosmological Microwave Background Radiation,Phys. Lett. B125(1983) 445. - 83 - [80] L.F. Abbott and M."},{"citing_arxiv_id":"2606.31324","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Madore, T. J. Hoyt, I. S. Jang, A. J. Lee, and K. A. Owens, Astrophys. J.985, 203 (2025), [Erratum: Astrophys.J. 993, 252 (2025)], arXiv:2408.06153 [astro-ph.CO]. [36] A. G. Riesset al., Astrophys. J.977, 120 (2024), arXiv:2408.11770 [astro-ph.CO]. [37] C. Voglet al., Astron. Astrophys.702(2025), 10.1051/0004-6361/202452910, arXiv:2411.04968 [astro-ph.CO]. [38] D. Scolnicet al., Astrophys. J. Lett.979(2025), 10.3847/2041-8213/ada0bd, arXiv:2409.14546 [astro-ph.CO]. [39] K. Saidet al., Mon. Not. Roy. Astron. Soc.539, 3627 (2025), arXiv:2408.13842 [astro-ph.CO]. [40] P. Boubel, M. Colless, K. Said, and L. Staveley-Smith, Mon. Not. Roy. Astron. Soc.533, 1550 (2024), arXiv:2408.03660 [astro-ph.CO]. [41] D. Scolnic, P."},{"citing_arxiv_id":"2606.30903","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmological Concordance in an Especially Opaque Universe: A Tentative Cosmological Detection of Physical Neutrino Mass in $\\Lambda$CDM","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T20:49:45+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Assuming τ=0.11±0.006 yields a 2σ positive neutrino mass detection (Σmν=0.10^{+0.04}_{-0.05} eV) and removes CMB-DESI tensions within ΛCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20434","ref_index":147,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Hubble tension: A decade review","primary_cat":"astro-ph.CO","submitted_at":"2026-06-18T16:12:11+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Pure early or late fixes to the Hubble tension are tightly constrained; remaining options are combined early-late interacting dark energy or new physics at the local-to-homogeneous transition.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"This is why BBN+BAO is often called an inverse distance ladder: instead of starting from local calibrators and climbing outward, one calibrates a high-redshift standard ruler and propagates the distance scale downward to inferH 0. Some of recent BAO+BBN results are:H 0 = 67.6±1.1 km s−1Mpc−1 [156],H 0 = 67.9± 1.1 km s−1Mpc−1 [157],H 0 = 68.6±1.1 km s −1Mpc−1 [147],H 0 = 67.35±0.97 km s −1Mpc−1 [94],H 0 = 68.19±0.99 km s −1Mpc−1 [150],H 0 = 67.58±0.91 km s −1Mpc−1 [158],H 0 = 67.6±1.0 km s −1Mpc−1 [159],H 0 = 67.42 +0.88 −0.94 km s−1Mpc−1 [143], andH 0 = 68.51± 0.58 km s−1Mpc−1 [160]. Again, these results strongly disfavor the idea that the Hubble ten- sion is merely a Planck-specific artifact of early-Universe observations."},{"citing_arxiv_id":"2606.09427","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Modifying $\\Lambda$CDM dynamics via out-of-equilibrium axions: reconciling SH0ES and DESI $H_0$ values","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T12:40:15+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A two-parameter model in which axion dark matter is driven out of equilibrium at late times fits SH0ES and DESI data with H0 ≈ 73 km/s/Mpc, but only when the SH0ES prior is included.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06495","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"What it takes to solve the Hubble tension through Modifications of Cosmological Recombination II: in light of ACT DR6 and DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Perturbative modifications to the electron mass m_e(z) resolve the Hubble tension with Planck+ACT CMB data but cannot when DESI DR2 BAO data are added due to lowered Omega_m.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"inferred from thePlancksatellite's cosmic microwave background (CMB) anisotropy data,H 0 = 67.36± 0.54 km s −1 Mpc−1 [1], while the local measurement is provided by the SH0ES collaboration,H 0 = 73.04± 1.04 km s−1 Mpc−1 [2], recently updated toH 0 = 73.17± 0.86 km s−1 Mpc−1 with an improved distance ladder cal- ibration [3]. The discrepancy between these two values now exceeds 5σ[4], making it unlikely to be a statisti- cal fluctuation and motivating extensive scrutiny of both systematic uncertainties and extensions to the standard cosmological model [5-141]. Among early-Universe solutions, modifications to the cosmological recombination history constitute a particu- larly well-motivated possibility. Recombination directly determines both the sound horizonr d and the detailed"},{"citing_arxiv_id":"2604.24761","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmological Impact of Redshift-Dependent Type Ia Supernovae Calibration","primary_cat":"astro-ph.CO","submitted_at":"2026-04-27T17:59:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A phenomenological redshift-dependent SNIa magnitude correction shows no evidence in ΛCDM but is preferred at 4.3σ with dynamical dark energy, reducing Hubble tension to 1.5σ.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Riess, Nature Astron.9, 1123 (2025), arXiv:2509.00359 [astro-ph.CO]. [2] N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), arXiv:1807.06209 [astro-ph.CO]. [3] E. Camphuiset al.(SPT-3G), Phys. Rev. D113, 083504 (2026), arXiv:2506.20707 [astro-ph.CO]. [4] A. G. Riesset al., Astrophys. J. Lett.934, L7 (2022), arXiv:2112.04510 [astro-ph.CO]. [5] L. Breuval, A. G. Riess, S. Casertano, W. Yuan, L. M. Macri, M. Romaniello, Y. S. Murakami, D. Scolnic, G. S. Anand, and I. Soszy' nski, Astrophys. J.973, 30 (2024), arXiv:2404.08038 [astro-ph.CO]. [6] M. Abdul Karimet al.(DESI), Phys. Rev. D112, 083515 (2025), arXiv:2503.14738 [astro-ph.CO]. [7] M. Kamionkowski and A. G. Riess, Ann. Rev. Nucl. Part."},{"citing_arxiv_id":"2604.16597","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Old Universe, Young SNe Ia: A Statistical Analysis of Type Ia Supernova Progenitor Age from 6,983 TITAN Host Galaxies, and Implications for Cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-04-17T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Large sample of SN Ia hosts shows young mean progenitor age of 3.5 Gyr and only 1.5 Gyr evolution, leading to negligible cosmological bias of 0.007 mag.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16564","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Observational tests of \\texorpdfstring{$\\Lambda(t)$}{Lambda(t)} cosmology in light of DESI DR2","primary_cat":"physics.gen-ph","submitted_at":"2026-04-17T10:06:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"MCMC constraints on two Lambda(t) models with DESI DR2, CC, and Pantheon+ data yield H0 ~72.5-73 km/s/Mpc, Omega_m0 near standard values in joint fits, and n~0.3 indicating mild deviation from LambdaCDM.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"vationally, a significant discrepancy has been reported in the measurement of Hubble constantH 0. Late-time measurements favor larger values ofH 0, while early- Universe estimates inferred from the CMB within the ΛCDM framework yield smaller values. This disagree- ment, known as theHubble tension, has been widely dis- cussed in the literature [13-20], with the current signif- icance exceeding 5σ[14, 21]. Additional anomalies and observational inconsistencies have also been reported in recent studies [22-28]. These theoretical and observa- tional challenges have motivated numerous investiga- tions into alternative cosmological scenarios that extend or modify the standardΛCDM framework. To explain cosmic acceleration, two broad classes of approaches have been widely explored in the literature."},{"citing_arxiv_id":"2604.13423","ref_index":88,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Into the Gompverse: A robust Gompertzian reionization model for CMB analyses","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T02:49:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A Gompertzian reionization model with three nuisance parameters demotes optical depth to a derived quantity, reducing its uncertainty by a factor of three and revealing potential neutrino mass tension in CMB analyses.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"For reference, DESI DR2 obtained Ω m = 0.3027±0.0036 andH 0 = 68.17±0.28 when combining DESI with CMB data [46]. Figure 2 contextualizes our findings in light of the DESI DR2 1σrange. We infer a larger value for the Hubble constant, very slightly more aligned with the SH0ES supernovae measurements calibrated using Cepheids (H 0 = 73.17±0.86 km s −1 Mpc−1 [88]). Likewise, our findings better align with the Chicago-Carnegie Hubble program using TRGB (Tip of the Red Giant Branch) stars for calibration [89]. In particular, their recent measurements using solely James Webb Space Telescope [90] data yieldH 0 = 68.81±2.22 [91] in good agreement with Eq. (5.1). The inclusion of BAO can also lead to smallerA s and largerτ reio."},{"citing_arxiv_id":"2604.12987","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T17:22:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Node-based reconstruction of cosmic expansion prefers stronger deceleration at z≈1.7 than smooth DE EoS parametrizations, isolating z~1.5-2 as a window where the latter may compress localized kinematic features permitted by current data.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"9, 373 (2000), arXiv:astro-ph/9904398. [2] P. J. E. Peebles and B. Ratra, Rev. Mod. Phys.75, 559 (2003), arXiv:astro-ph/0207347. [3] E. J. Copeland, M. Sami, and S. Tsujikawa, Int. J. Mod. Phys. D15, 1753 (2006), arXiv:hep-th/0603057. [4] S. Weinberg, Rev. Mod. Phys.61, 1 (1989). [5] A. G. Riesset al., Astrophys. J. Lett.934, L7 (2022), arXiv:2112.04510 [astro-ph.CO]. [6] L. Breuval, A. G. Riess, S. Casertano, W. Yuan, L. M. Macri, M. Romaniello, Y. S. Murakami, D. Scolnic, G. S. Anand, and I. Soszy' nski, Astrophys. J.973, 30 (2024), arXiv:2404.08038 [astro-ph.CO]. [7] N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [8] S. Alamet al."},{"citing_arxiv_id":"2602.11936","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"work: a community consensus report on the measure- ment of the Hubble constant at 1% precision (2025), arXiv:2510.23823 [astro-ph.CO]. [26] V. Poulin, T. L. Smith, T. Karwal, and M. Kamionkowski, Phys. Rev. Lett.122, 221301 (2019), arXiv:1811.04083 [astro-ph.CO]. [27] T. Karwal and M. Kamionkowski, Phys. Rev. D94, 103523 (2016), arXiv:1608.01309 [astro-ph.CO]. [28] J. C. Hill, E. McDonough, M. W. Toomey, and S. Alexander, Phys. Rev. D102, 043507 (2020), arXiv:2003.07355 [astro-ph.CO]. [29] M. Kamionkowski and A. G. Riess, Ann. Rev. Nucl. 14 Part. Sci.73, 153 (2023), arXiv:2211.04492 [astro- ph.CO]. [30] M. M. Ivanov, E. McDonough, J. C. Hill, M. Simonović, M.W.Toomey, S.Alexander,andM.Zaldarriaga,Phys. Rev."},{"citing_arxiv_id":"2512.02526","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2511.09467","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Revisiting the Hubble tension problem in the framework of holographic dark energy","primary_cat":"astro-ph.CO","submitted_at":"2025-11-12T16:39:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"HDE models with future event horizon IR cutoff partially ease the Hubble tension while Hubble-scale cutoffs do not, consistent across six models and multiple BAO/SN/CMB combinations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"sults from the Dark Energy Spectroscopic Instrument (DESI) collaboration [8, 9] provided further evidence for deviation from ΛCDM. Using the combination of DESI Data Release 2 (DR2) and CMB data, the DESI found a 3.1σCL preference for the Chevallier-Polarski-Linder (CPL) model [10, 11] over ΛCDM. Moreover, after adding the PantheonPlus [12], Union3 [13], or DESY5 [14] type Ia supernovae (SN) dataset into the combination, the ∗ lijx389@mail2.sysu.edu.cn † wangshuang@mail.sysu.edu.cn; (corresponding author) preference is 2.8σ, 3.8σor 4.2σ, respectively. These de- viations from the cosmological constant have sparked ex- tensive debates on dynamical dark energy (DE), includ- ing scalar field DE models [15-22], interacting DE models"},{"citing_arxiv_id":"2510.18741","ref_index":36,"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":"measurement of the Hubble-Lemaître constant from Type II supernovae, Mon. Not. Roy. Astron. Soc.514, 4620 (2022), 2203.08974. [35] Y. S. Murakami, A. G. Riess, B. E. Stahl, W. D. Ken- worthy, D.-M. A. Pluck, A. Macoretta, D. Brout, D. O. Jones, D. M. Scolnic, and A. V. Filippenko, Leveraging SN Ia spectroscopic similarity to improve the measure- ment of H0, JCAP11, 046, 2306.00070. [36] L. Breuval, A. G. Riess, S. Casertano, W. Yuan, L. M. Macri, M. Romaniello, Y. S. Murakami, D. Scolnic, G. S. Anand, and I. Soszyński, Small Magellanic Cloud Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder, Astrophys. J.973, 30 (2024), 2404.08038. [37] W. L. Freedman, B. F. Madore, T. J. Hoyt, I."},{"citing_arxiv_id":"2510.18320","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The implications of inflation for the last ACT","primary_cat":"astro-ph.CO","submitted_at":"2025-10-21T06:09:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A parameterized slow-roll model and a new exponential f(R) inflation model are constrained by P-ACT-LB-BK18 data, with the latter aligning to the ACT scalar spectral index preference in both standard and EDE frameworks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.22066","ref_index":86,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2503.14738","ref_index":131,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"do not report joint constraints on parameters from any combination of DESI and SNe data. However, as with the CMB, these apparent parameter differences poten- tially indicate that DESI and at least some of the SNe datasets cannot be consistently fit except with models that have greater freedom in the background evolution, as described in the next section (see also [131]). VII. DARK ENERGY Probing the behavior and nature of dark energy is the primary goal of DESI. The question of perhaps greatest interest, and the one that BAO measurements can best il- luminate, is the value of the equation-of-state parameter w = P/(ρc2), and its possible evolution with time. To ex- amine this we will primarily use the so-called Chevallier-"},{"citing_arxiv_id":"2404.03002","ref_index":237,"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":"Condon et al., The Megamaser Cosmology Project. XIII. Combined Hubble Constant Constraints , ApJ 891 (2020) L1 [ 2001.09213]. [236] A.G. Riess et 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 (2022) L7 [ 2112.04510]. [237] L. Breuval, A.G. Riess, S. Casertano, W. Yuan, L.M. Macri, M. Romaniello et al., Small Magellanic Cloud Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder , arXiv e-prints (2024) arXiv:2404.08038 [ 2404.08038]. [238] W.L. Freedman, B.F. Madore, T. Hoyt, I.S. Jang, R. Beaton, M.G. Lee et al., Calibration of"},{"citing_arxiv_id":"2402.07716","ref_index":37,"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":"Owens, Status Report on the Chicago-Carnegie Hubble Program (CCHP): Three In- dependent Astrophysical Determinations of the Hubble Constant Using the James Webb Space Telescope (2024), 2408.06153. [36] A. G. Riess et al., JWST Validates HST Distance Mea- surements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H0 (2024), 2408.11770. [37] C. Vogl et al., No rungs attached: A distance-ladder free determination of the Hubble constant through type II supernova spectral modelling (2024), 2411.04968. [38] D. H. Gao, Q. Wu, J. P. Hu, S. X. Yi, X. Zhou, and F. Y. Wang, Measuring Hubble constant using localized and unlocalized fast radio bursts (2024), 2410.03994. [39] D. Scolnic et al., The Hubble Tension in our own Back-"}],"limit":50,"offset":0}