{"total":19,"items":[{"citing_arxiv_id":"2605.08080","ref_index":83,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"CMB Limits on the Absorption of Light Vector and Axial-Vector Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-05-08T17:59:28+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Planck CMB data set upper limits on vector and axial-vector dark matter-electron couplings for masses 100 eV to 100 keV via energy injection from inelastic scattering and hydrogen absorption.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.21671","ref_index":100,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Saturation Mechanisms in the Interacting Dark Sector","primary_cat":"astro-ph.CO","submitted_at":"2026-04-23T13:36:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Nonlinear dark-sector interaction models with a half-saturation sparseness scale are observationally preferred over their linear counterparts at >95% confidence for two of three cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19922","ref_index":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measuring neutrino mass and asymmetry through galaxy pairwise peculiar velocity","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T19:01:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Galaxy pairwise peculiar velocities from Cosmicflows-4 yield M_ν = 0.24^{+0.34}_{-0.18} eV and η² = 2.14^{+0.30}_{-0.32} (7σ non-zero asymmetry) in the CMB framework, consistent with prior Planck results.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19198","ref_index":64,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmological constraints on TeV-scale dark matter subcomponents decaying between recombination and reionisation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T08:07:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Future 21-cm observations may constrain TeV-scale decaying dark matter subcomponents more tightly than CMB data for lifetimes above 10^15 s, with strongest sensitivity for neutrino decay channels due to differences in injected electromagnetic energy spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16564","ref_index":80,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.13535","ref_index":169,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Double the axions, half the tension: multi-field early dark energy eases the Hubble tension","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T06:29:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Two-field axion-like early dark energy reduces Hubble tension to 1.5 sigma residual and improves high-ell CMB fits over single-field models.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Distance Network [11], which we refer to as H0DN. We refer to the CMB dataset as \"P\", the combination with SNeIa and BAO data as \"PD\", and the combination of all data including the H0DN prior as \"PDH0\". We perform a Bayesian analysis via Markov Chain Monte Carlo (MCMC) runs using theMontePythonsam- pler [167, 168], and analyzing our MCMC chains via the GetDistpackage [169]. Bayesian analyses of EDE are known to be susceptible to prior volume effects [170-174], which can shift the inferredH 0 (towards either larger or smaller values) independently of any genuine change in quality of fit. We therefore complement our MCMC anal- ysis with a frequentist profile likelihood (PL) approach using theProcolipackage [175] to determine both the"},{"citing_arxiv_id":"2604.11865","ref_index":50,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Beyond the Cosmological Constant: Breaking the Geometric Degeneracy of $ f(Q) $ cosmology via Redshift-Space Distortions","primary_cat":"gr-qc","submitted_at":"2026-04-13T16:16:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hybrid f(Q) cosmology with a 1/Q term is forced into background degeneracy with LambdaCDM but breaks it in the growth sector, yielding moderate preference over LambdaCDM when RSD data are included while leaving the background unchanged.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.08530","ref_index":126,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.04867","ref_index":104,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measurement of the galaxy-velocity power spectrum of DESI tracers with the kinematic Sunyaev-Zeldovich effect using DESI DR2 and ACT DR6","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T17:16:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR2 and ACT DR6 data yield 17σ LRG-velocity, 8.3σ ELG-velocity, and 6.8σ QSO-velocity detections plus a 3.1σ velocity-velocity signal, producing f_NL^loc = 15.9_{-34.4}^{+34.6} from the velocity field.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.04408","ref_index":96,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T04:19:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Analysis of galaxy cluster and supernova data reveals a ~2σ directional variation in the Hubble constant, robust across calibration methods and aligned with the CMB dipole.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.03756","ref_index":80,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Is the $w_0w_a$CDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?","primary_cat":"astro-ph.CO","submitted_at":"2026-04-04T15:05:07+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Planck PR4 CMB data mildly favors dynamical dark energy, but this preference weakens when accounting for possible excess smoothing, indicating the signal may partly arise from data processing issues.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.03167","ref_index":110,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Mapping the redshift drift at various redshifts through cosmography","primary_cat":"astro-ph.CO","submitted_at":"2026-04-03T16:44:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Cosmographic Taylor and Padé models fitted to Pantheon+SH0ES+GRB+DESI BAO data yield redshift drift predictions compatible with ΛCDM and ω0ω1CDM at 1-2σ, with mock drift data tightening q0 and j0 bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.02204","ref_index":76,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Non-minimally coupled quintessence with sign-switching interaction","primary_cat":"astro-ph.CO","submitted_at":"2026-04-02T15:57:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new quintessence model with non-minimal coupling produces an effective sign-switching interaction that fits current data better than LambdaCDM or w0waCDM and accounts for late-time dark energy weakening without phantom crossing.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.27616","ref_index":98,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Model-independent test of the cosmic distance duality relation with recent observational data","primary_cat":"astro-ph.CO","submitted_at":"2026-03-29T10:21:42+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Two model-independent methods applied to latest SN and BAO data find the cosmic distance duality relation consistent with observations within 1 sigma and no evidence of violation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.09153","ref_index":75,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Euclid preparation. XCVI. Cosmology Likelihood for Observables in Euclid (CLOE). 3. Inference and Forecasts","primary_cat":"astro-ph.CO","submitted_at":"2025-10-10T08:57:09+00:00","verdict":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":"2506.20707","ref_index":212,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field","primary_cat":"astro-ph.CO","submitted_at":"2025-06-25T18:00:00+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SPT-3G delivers the most precise CMB EE and TE spectra at high multipoles to date, giving LCDM parameters with H0 = 66.66 ± 0.60 km/s/Mpc from ground-based data alone and reaching Planck-level constraints when combined with ACT.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14738","ref_index":127,"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":"method","top_context_polarity":"use_method","context_text":"tributions are symmetric and the 68% minimal credible interval when they are not. Where only limits on param- eter values can be determined, upper or lower bounds are quoted at the 68% level, except forP mν where we quote the 95% upper bound to ensure comparability with previous work. In order to determine the best fit points and the corre- sponding χ2 we use the iminuit [127] algorithm starting from the maximum a posteriori (MAP) points of each of the chains in the MCMC sampling. When comparing the fits of two different models we compare the quan- tity ∆ χ2 MAP ≡ − 2∆ lnL representing twice the differ- ence in the negative log posteriors at the maximum pos- terior points for each model. This measure accounts for the contribution of any non-uniform priors when evalu-"},{"citing_arxiv_id":"2404.03002","ref_index":186,"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":"method","top_context_polarity":"use_method","context_text":"weighted chain length divided by the autocorrelation length for all parameters) to be≳ 103 to achieve percent precision on the moments of the marginal posteriors. In the case of symmetric 1D marginalised posteriors we report the mean and standard deviation of the samples, while the 68% minimal credible interval is quoted in other cases, except when otherwise stated. We - 16 - use getdist13 [186] to derive the constraints presented in this paper. Where appropriate, we also compute the best-fit with the iminuit [187, 188] algorithm, as implemented in cobaya, starting from the four maximum a posteriori (MAP) points of the corresponding four MCMC chains. In our analysis, we use ∆χ2 MAP ≡ −2∆ logL, defined to represent the difference (times −2) of log-posteriors at the maximum posterior points."},{"citing_arxiv_id":"2005.05290","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cobaya: Code for Bayesian Analysis of hierarchical physical models","primary_cat":"astro-ph.IM","submitted_at":"2020-05-11T17:49:03+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Cobaya is a modular Bayesian analysis code that exploits model interdependencies via automatic caching and a novel parameter-blocking algorithm to minimize sampling cost.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}