{"total":44,"items":[{"citing_arxiv_id":"2605.21456","ref_index":117,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Negative neutrino mass or negative dark energy?","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:46:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A sign-switching dark energy model (Λ_s CDM) recovers positive effective neutrino masses (0.055 ± 0.050 eV) consistent with oscillation data, unlike ΛCDM which prefers negative values (-0.075 eV), for DESI DR2 + CMB + supernova fits with z_† > 2.4.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"In the presence of massive neutrinos, however, the actual growth is scale dependent, so Eqs.(15) and (16) should be read as heuristic guidance rather than as the numerical model used in the analysis. The representative spectra shown in Fig. 2 are computed numerically with the Boltzmann solver CAMB [116], while the parameter inference reported in Section VI uses a modified version ofCLASS[117, 118] introduced in Section V. What kind of late-time modification can replace a neg- ative effective neutrino mass?Based on the discussion above, we summarize the requirements that a DE model should satisfy in order to alleviate the neutrino mass ten- sion. At the background level, the model must satisfy two conditions. For fixedΩmh2 and the accurately mea-"},{"citing_arxiv_id":"2605.21436","ref_index":151,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:26:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validates redshift-space power spectrum and bispectrum analysis on Abacus-PNG mocks to recover unbiased f_NL constraints for Euclid spectroscopic sample.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"against other public tools for Fourier-space modelling and pa- rameter inference onN-body simulations (see Euclid Collabo- ration: Pezzotta et al. 2024; Euclid Collaboration: Pardede et al. 2026, for comparisons against Euclid Flagship 1 simulations). CosmoSIS-gClustalso underpins the newCLASS-OneLoop Article number, page 9 of 30 A&A proofs:manuscript no. main (Linde et al. 2024) extension toCLASS(Lesgourgues 2011). For local PNG, further validation of the Abacus halo catalogues (Hadzhiyska et al. 2024) is presented in the companion paper (Linde & Moradinezhad in prep.). The package consists of two libraries: (i)gclust, which pro- vides the theoretical predictions; and (ii)gstats, which com- putes the corresponding likelihoods. Withingclust, the galaxy power spectrum and bispectrum are computed at one-loop and"},{"citing_arxiv_id":"2605.20748","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing late-time deviations from $\\Lambda$CDM with a quadratic dark energy expansion","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T05:49:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The QDEE model fits combined cosmological datasets better than Lambda CDM, shifts the Hubble constant higher, and shows strong Bayesian evidence in its favor.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18716","ref_index":65,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Recoupled Dark Radiation reconciling CMB and DESI BAO measurements","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T17:47:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An interacting sterile neutrino component via pseudoscalar mediator reconciles CMB and DESI DR2 BAO measurements with 2.7 sigma preference and reduces H0 tension to 2.4 sigma.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13967","ref_index":44,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"When galaxies burst: enhanced shot-noise for line-intensity mapping in the JWST era","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bursty high-redshift star formation boosts LIM shot-noise by line-dependent factors B_λ of 2.5-7 at z~6 via convolution of SFR correlations with SPS kernels, improving auto-spectrum detectability while degrading clustering measurements.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10116","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Reionization History and Neutrino Mass","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T07:32:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reionization histories with higher total optical depth can move the best-fit neutrino mass sum to positive values around 0.06 eV within 95% confidence from CMB and BAO data.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We introduce one benchmark reionization history and three astrophysically allowed histories, as shown in the upper left panel of Fig. 1. The benchmark case is the fiducial reionization model implemented in CLASS [14], withτleft as a free parameter. For illustration, the blue dashed curve in the upper left panel of Fig. 1 shows this model for the particular choiceτ≃0.061. It uses the default tanh-like reionization parametrization in CLASS [16], which contains one tanh transition for hydrogen reionization and another tanh transition for the second ionization of helium at low redshift. The other three history profiles are taken from Ref. [17] and are denoted as Low-τEoR, Representative EoR, and High-τEoR, according to their resulting optical depths. They are shown by the purple, red, and orange solid lines in the upper left panel of Fig."},{"citing_arxiv_id":"2605.08907","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"method","top_context_polarity":"use_method","context_text":"• BK18: BB data from BICEP/Keck XIII survey [33]. When this dataset is com- bined with SPTpolBB, we restrict the latter to the multipole range ℓ > 400 to avoid double counting of information. 4 Note that, except for BK18, we use the lite, i.e. foreground-marginalised [43, 44] versions of the likelihoods. For the numerical implementation, we modified the Boltzmann code CLASS [45, 46] to incorporate V-modes for each of the above mentioned ICs and perform our com- putations (which we make publicly available 5). We use the Bayesian analysis code COBAYA [47-49]6 to run our Markov chains Monte Carlo (MCMC), and consider chains to be converged when the Gelman-Rubin criterion [50] is R − 1 ≲ 0.05. In addition to τreio mentioned above, we sample over the energy densities of baryons (ωb) and cold dark"},{"citing_arxiv_id":"2605.05323","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Primordial Magnetic Fields at Cosmic Dawn: 21-cm Forecasts with HERA and SKA","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T18:00:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Primordial magnetic fields enhance low-mass halo abundance at Cosmic Dawn, advancing Lyman-alpha coupling, X-ray heating and reionization and imprinting detectable signatures on global and fluctuating 21-cm signals observable by HERA and SKA.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"(1998). [54] K. Subramanian and J. D. Barrow, Magnetohydrody- namics in the early universe and the damping of nonlinear alfv' en waves, Phys. Rev. D58, 083502 (1998). [55] T. Kahniashvili, A. G. Tevzadze, and B. Ratra, Phase Transition Generated Cosmological Magnetic Field at Large Scales, Astrophys. J.726, 78 (2011), arXiv:0907.0197 [astro-ph.CO]. [56] J. Lesgourgues, The cosmic linear anisotropy solving system (class) i: Overview (2011), arXiv:1104.2932, arXiv:1104.2932 [astro-ph.IM]. [57] D. Blas, J. Lesgourgues, and T. Tram, The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation schemes, JCAP07, 034, arXiv:1104.2933 [astro-ph.CO]. [58] J. Lesgourgues, The cosmic linear anisotropy solving sys-"},{"citing_arxiv_id":"2604.26541","ref_index":128,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The End of the First Act: Spectral Running, Interacting Dark Radiation, and the Hubble Tension in Light of ACT DR6 Data","primary_cat":"astro-ph.CO","submitted_at":"2026-04-29T11:12:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Including spectral running α_s, β_s and self-interacting dark radiation relaxes the ACT DR6 bound on ΔN_eff to <0.58 and lowers the Hubble tension to 2.2σ with three extra parameters.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"modifies the evolution of perturbations relative to the pure SIDR case, while the background evolution is identical. In particular, the DRMD model predicts a characteristic dark acoustic oscillation feature imprinted on matter perturbations [41]. B. Data and analysis We employ a joint Planck-ACT CMB compilation (temperature, polarization, and lens- ing) [2, 127], Pantheon+ SN data [128, 129], and DESI DR2 BAO data [12, 130]. The CMB dataset combines theACT DR6 litelikelihood with Planck 2018 data (with cutsℓ≤1000 andℓ≤600 for TT and (TE, EE) spectra, respectively), including the SRoll2 low-ℓpolariza- tion likelihood [131], and is supplemented by ACT DR6 CMB lensing data [132, 133] (in the actplanck baselinevariant). We further use the Pantheon+ SN dataset in itsuncalibrated"},{"citing_arxiv_id":"2604.18581","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"If at First You Don't Succeed, Trispectrum: I. Estimating the Matter Power Spectrum Covariance with Higher-Order Statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T17:59:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Estimators from squeezed bispectrum and collapsed trispectrum recover unbiased small-scale matter power spectrum covariance at the percent level using 25 Quijote simulations.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"strong separation of scales underlying these observables, it may be possible to calculate the required covariances (semi-)analytically (see, e.g., Refs. [ 9, 53]). We leave a detailed investigation of approaches that circumvent the need for a trispectrum covariance estimate to future work. Equipped with a likelihood and covariance, we sample from the parameter posterior using the emcee package [54] assuming wide uniform priors, −106 (Mpc/h)3 <¯ak 0,¯ak′ b 0 <10 6 (Mpc/h)3, −109 (Mpc/h)6 < ¯T kb,k′ b 0 /V <10 9 (Mpc/h)6, where V is the simulation volume. We assess convergence using the Gelman-Rubin statistic [55], requiring |R− 1|< 0.01. IV. RESULTS Fig. 2 shows the main summary statistics considered in this work: the long-wavelength power spectrum, the"},{"citing_arxiv_id":"2604.18007","ref_index":51,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"[49] D. P. Finkbeiner, S. Galli, T. Lin and T. R. Slatyer,Searching for dark matter in the cmb: A compact parametrization of energy injection from new physics,Phys. Rev. D85(Feb., 2012) 043522, [1109.6322]. [50] J. Lesgourgues,The cosmic linear anisotropy solving system (class) i: Overview,arXiv e-prints (Apr., 2011) arXiv:1104.2932, [1104.2932]. [51] D. Blas, J. Lesgourgues and T. Tram,The cosmic linear anisotropy solving system (class). part ii: Approximation schemes,J. Cosmology Astropart. Phys.2011(July, 2011) 034, [1104.2933]. [52] T. R. Slatyer, N. Padmanabhan and D. P. Finkbeiner,Cmb constraints on wimp annihilation: Energy absorption during the recombination epoch,Phys. Rev. D80(Aug., 2009) 043526,"},{"citing_arxiv_id":"2604.13547","ref_index":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Reconstructing inflationary features on large scales using genetic algorithm","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T06:50:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Genetic algorithm reconstructs single-field inflationary models with features in the scalar power spectrum that fit Planck 2018 CMB data better by Δχ² ≲ -10 and suggest alternative background parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[48] N. Aghanimet al.(Planck), Astron. Astrophys.641, A5 (2020), arXiv:1907.12875 [astro-ph.CO]. [49] J. Lesgourgues, (2011), arXiv:1104.2932 [astro-ph.IM]. [50] D. Blas, J. Lesgourgues, and T. Tram, JCAP07, 034 (2011), arXiv:1104.2933 [astro-ph.CO]. [51] D. K. Hazra, L. Sriramkumar, and J. Martin, JCAP 05, 026 (2013), arXiv:1201.0926 [astro-ph.CO]. [52] T. S. Bunch and P. C. W. Davies, Proc. Roy. Soc. Lond. A357, 381 (1977). [53] T. S. Bunch and P. C. W. Davies, Proc. Roy. Soc. Lond. A360, 117 (1978). [54] T. S. Bunch and P. C. W. Davies, J. Phys. A11, 1315 (1978). [55] P. A. R. Adeet al.(BICEP, Keck), Phys. Rev. Lett. 127, 151301 (2021), arXiv:2110.00483 [astro-ph.CO]. [56] M. Affenzeller, S. Winkler, S."},{"citing_arxiv_id":"2604.13535","ref_index":160,"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":"critical redshift. TheN ax EDE fields are taken to be non-interacting, and their individual perturbations obey the same equations of the standard, single-field EDE model [97]. We implement these equations in the publicly availablemAxiCLASScode, 1 a modified version of the ear- lierAxiCLASS[94, 95, 158, 159], 2 itself an extension of theCLASS 3 Boltzmann solver [160, 161]. 1 https://github.com/marcobeIIa/mAxiCLASS 2 https://github.com/PoulinV/AxiCLASS 3 https://github.com/lesgourg/class_public arXiv:2604.13535v1 [astro-ph.CO] 15 Apr 2026 2 Our analysis compares models withN ax = 1,2,3 EDE fields. Each of these is allowed to be dynamical in a distinct redshift bin within the overall range log 10 zc ∈ [3,4.5]."},{"citing_arxiv_id":"2604.12032","ref_index":113,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on Coupled Dark Energy in the DESI Era","primary_cat":"astro-ph.CO","submitted_at":"2026-04-13T20:21:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New cosmological data mildly favor a small coupling between dark matter and a scalar dark energy field at |β| ≈ 0.03 while allowing an effective phantom-crossing equation of state.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"field is presented in terms of the following dimensionless quantity,φ ini ≡κϕ ini/ √ 3. In the last three rows we report the minimum values ofχ 2,χ 2 min, the differences ∆AIC≡AIC Λ −AIC CDE and the level of exclusion of ΛCDM obtained through a likelihood-ratio test,E ΛCDM. cosmological observables involved in the fitting analyses. We employ the codeCobaya6 [113] to perform the exploration of the parameter space with Monte Carlo runs and theGetDist 7 package [114] for the processing of the Monte Carlo Markov chains (MCMC) and the extraction of the parameter constraints. We constrain the CDE models with constant and PR potentials, considering for the latter two distinctive cases with positive and negative couplings, and compare our fitting results with those obtained with the ΛCDM, which we"},{"citing_arxiv_id":"2604.12020","ref_index":76,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Beyond the Standard Model of Cosmology: Testing new paradigms with a Multiprobe Exploration of the Dark Universe","primary_cat":"astro-ph.CO","submitted_at":"2026-04-13T20:05:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Proposes primordial black holes from modified small-scale fluctuations and entropic acceleration in expanding spacetime as explanations for dark matter and dark energy.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"within the Legacy Survey of Space and Time (LSST) Consortium in the Vera Rubin Observatory, a new microlensing survey with LSST and the Nancy Roman space telescope (NRST) [75]. This combined photometric (LSST) and astrometric (NRST) survey will allow us to break the degeneracies between mass and distance in the Einstein radius and thus half-crossing times [76]. I further proposed that we use spectroscopy of the source in order to distinguish the type of dark compact object that acted as lens. This may allow us to eventually detect the QCD peak of the THM in the solar-mass range, with a sub-solar mass tail that would be proof of its primordial origin. C. Observational constraints on General Relativistic Entropic Acceleration"},{"citing_arxiv_id":"2604.07327","ref_index":60,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Primordial magnetic fields in the light of upcoming post-EoR Lyman-$\\alpha$ and 21-cm observations","primary_cat":"astro-ph.CO","submitted_at":"2026-04-08T17:44:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts show DESI-like and SKA1-Mid observations could constrain primordial magnetic field amplitude and spectral index to roughly 10% precision via 21cm auto-spectrum and Lyα-21cm cross-spectrum.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"01 hMpc −1 and kmax = 5 hMpc −1 are excluded from the Fisher analysis. The instrumental specifications adopted for PUMA in this work are summarized in Table 1. 3.2.2 SKA1-Mid (Single-Dish Mode) The SKA1-Mid survey is designed to operate in the SD mode across two frequency bands, with SKA1-Mid Band 1 covering the redshift range0.35 < z < 3.05and SKA1-Mid Band 2 covering0 .10 < z < 0.49[ 60, 85]. In single-dish mode, each dish operates independently as a total-power radiometer, mapping the sky by scanning across it. The individual maps from all dishes are subsequently co-added, reducing the thermal noise by a factor√Ndish relative to a single dish. Unlike the interferometer case, the thermal noise in single-dish mode is approximately isotropic in Fourier space to leading order, since there is no baseline density"},{"citing_arxiv_id":"2604.06261","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Late-Transition Interacting Thawer Dark Energy: Physics and Validation","primary_cat":"gr-qc","submitted_at":"2026-04-07T01:15:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LTIT is a constrained interacting dark energy framework with late-activating variable coupling to CDM that keeps pre-recombination effects below 0.4 percent while permitting sub-percent to several-percent late-time shifts in growth.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.05095","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A generic $\\omega_b$ tension in early-time solutions to the Hubble tension","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T18:48:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Early-time Hubble tension solutions generically raise the preferred baryon density ω_b, conflicting with BBN deuterium constraints and producing poorer fits to CMB, BAO, supernova, and BBN data than ΛCDM.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"A 4 per cent distance measure at z=0.15,\" Monthly Notices of the Royal Astronomical Society449, 835-847 (2015). [43] Sven G¨ untheret al., \"OL 'E - online learning emulation in cosmology,\" (2025), arXiv:2503.13183 [astro-ph.CO]. [44] Julien Lesgourgues, \"The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview,\" (2011), arXiv:1104.2932 [astro-ph.IM]. [45] Diego Blas, Julien Lesgourgues, and Thomas Tram, \"The Cosmic Linear Anisotropy Solving System (CLASS). part II: Approximation schemes,\" Journal of Cosmology and Astroparticle Physics2011, 034-034 (2011). [46] Julien Lesgourgues, \"The Cosmic Linear Anisotropy Solving System (CLASS) III: Comparision with CAMB for LambdaCDM,\" (2011), arXiv:1104.2934 [astro-"},{"citing_arxiv_id":"2604.03167","ref_index":72,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"by considering measurements of the evolution of cosmic redshift through the use of quasar's spectra [6]. map the interval 2≤z≤5 with GRBs pushing over z≥5. The constraints on the parameters are de- rived by modifying the Cosmic Linear Anisotropy Solving System (CLASS) code [69-71] and performing a Monte Carlo Markov chain (MCMC) analysis adopting the MontePythonsampler [72, 73]. Specifically, we follow the strategy outlined in Refs. [11, 12], precisely, - we do preliminary MCMC runs to constrain the Hubble, deceleration and jerk parameters with the adoption of SNeIa+GRB (Analysis 1) and with SNeIa+GRB+DESI-BAO (Analysis 2) to assess the impact of the BAO data on the parameters; - we substitute for each analysis the constrained pa-"},{"citing_arxiv_id":"2603.26560","ref_index":135,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exploring the interplay of late-time dynamical dark energy and new physics before recombination","primary_cat":"astro-ph.CO","submitted_at":"2026-03-27T16:25:41+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":"is a reflection of the insensitivity of the DE parameters to the specific calibration used in the analysis. Therefore, the decrease in significance of the preference for dynamical dark energy arises primarily from discarding the additional information provided by the CMB under the assumption of standard recombination. This result resonates well with that of Ref. [135]. Even in this conservative approach13 - where no specific model of early-time new physics is assumed - the fact that Ω0 m is well determined by late-time observables implies an increase in Ω0 mh2 when early-Universe physics is invoked to reduce the sound horizon with the aim of explaining the values ofH 0 preferred by SH0ES or CCHP 14. This provides further motiva-"},{"citing_arxiv_id":"2603.13053","ref_index":80,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A unified harmonic framework for dark siren cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-03-13T15:03:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The GW-galaxy cross-correlation method, unified with spectral sirens in a harmonic framework, can measure H0 to 1% and Omega_m to 5% precision with 2 years of data from next-generation detectors like Einstein Telescope and Cosmic Explorer.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A. Scharf, and O. Lahav, A spherical harmonic approach to redshift distortion and a measure- ment of Omega(0) from the 1.2-Jy IRAS Redshift Sur- vey, MNRAS266, 219 (1994), arXiv:astro-ph/9309027 [astro-ph]. [79] A. F. Heavens and A. N. Taylor, A spherical harmonic analysis of redshift space, MNRAS275, 483 (1995), arXiv:astro-ph/9409027 [astro-ph]. [80] S. Dodelson, V. K. Narayanan, M. Tegmark, R. Scran- ton, T. Budav' ari, A. Connolly, I. Csabai, D. Eisenstein, J. A. Frieman, J. E. Gunn, L. Hui, B. Jain, D. Johnston, S. Kent, J. Loveday, R. C. Nichol, L. O'Connell, R. Scoc- cimarro, R. K. Sheth, A. Stebbins, M. A. Strauss, A. S. Szalay, I. Szapudi, M. S. Vogeley, I. Zehavi, J. An- nis, N. A. Bahcall, J."},{"citing_arxiv_id":"2603.07398","ref_index":62,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Study of the cosmological tensions and DESI-DR2 in the framework of the Little Rip model","primary_cat":"astro-ph.CO","submitted_at":"2026-03-08T01:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"The Little Rip model reduces the Hubble tension below 3σ with CMB plus BAO data but only improves the statistical fit to CMB data alone per Bayes factors, and shifts toward quintessence behavior when DESI-DR2 is included.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.21432","ref_index":85,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological analysis of the DESI DR1 Lyman alpha 1D power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-01-29T09:08:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR1 Lyman-alpha data yields Δ²★=0.379±0.032 and n★=-2.309±0.019 at k★=0.009 km⁻¹s and z=3, sharpening N_eff, α_s, and β_s constraints by factors of 1.18-1.90 when combined with other probes.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"However, as shown in sec- tion 5.3, inaccuracies due to the limited resolution of the simulations do not bias cosmological constraints. All the simulations begin atz= 99 from initial conditions generated withMP-GenIC [84] using baryon and dark matter particles initialized on offset grids with species-specific transfer functions calculated employingCLASS[85, 86], displacements computed using the Zel'dovich approximation, and same distribution of Fourier phases. This configuration is accurate over the range of scales and redshifts accessed by DESI measurements [84, 87]. We refer the reader to [23, 88] for more details about these simulations. P1D measurements are sensitive to the small-scale amplitude and logarithmic slope of"},{"citing_arxiv_id":"2601.02886","ref_index":44,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The velocity coherence scale: a novel probe of cosmic homogeneity and a potential standard ruler","primary_cat":"astro-ph.CO","submitted_at":"2026-01-06T10:13:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The velocity coherence scale R_v marks the onset of statistical homogeneity, is redshift-independent in comoving coordinates, and connects directly to the matter-radiation equality scale k_eq in standard cosmology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.14455","ref_index":71,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Isocurvature-induced features in multi-field Higgs-$R^2$ inflation","primary_cat":"astro-ph.CO","submitted_at":"2025-12-16T14:44:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical multi-field analysis of Higgs-R² inflation with kinetic mixing identifies two regimes: moderate ξ_h produces localized features in the curvature power spectrum via isocurvature transfer, while weak ξ_h leaves a nearly featureless spectrum with residual isocurvature.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.20757","ref_index":135,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses","primary_cat":"astro-ph.CO","submitted_at":"2025-11-25T19:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reanalysis of DESI full-shape clustering data tightens constraints on neutrino mass, spatial curvature, and dark energy equation-of-state parameters relative to BAO-only results.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"parametrized by Ω k; non-minimal neutrino masses, described by Mν ≡ P mν; dynamical dark energy, with equation- of-state w(a) = w0 + wa(1 −a ). When the total neutrino mass is varied we assume three degenerate mass eigenstates 5 and impose a physical prior Mν ≥ 0; when it is not varied, Mν is fixed to the minimal value of 0 .06 eV, modeled as a single massive and two massless states. The linear-order evolution of these is computed using theclasscode [135], which is sufficient to describe the CMB, BAO and SNe observables. This depends on six baseline parameters: H0, ωc ≡ Ωch2, ωb ≡ Ωbh2, As, ns, τ (describing the expansion rate, physical dark matter and baryon density, primordial amplitude and slope and reionization optical depth respectively), as well as those describing the above extensions. To reduce parameter degeneracies, we fix τ to the CMB best-fit and impose a BBN prior on ωb and a wide prior on"},{"citing_arxiv_id":"2511.00822","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The CatWISE2020 Quasar dipole: A Reassessment of the Cosmic Dipole Anomaly","primary_cat":"astro-ph.CO","submitted_at":"2025-11-02T06:21:28+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reassessment of the CatWISE2020 quasar dipole with comprehensive simulations lowers the anomaly significance from 4.9σ to 3.27–3.63σ but leaves it unexplained by clustering or mask effects alone.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.17977","ref_index":104,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Growth of Structure in Multi-species Wave Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2025-10-20T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Derives the power spectrum evolution and cross-spectra for arbitrary multi-species wave and particle dark matter, incorporating free-streaming, Jeans scales, and intrinsic fluctuations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.14888","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"Pakmor, O. Zier, and M. Reinecke, Simulating cosmicstructureformationwiththeGADGET-4code,Monthly Notices of the Royal Astronomical Society506, 2871 (2021), arXiv:2010.03567 [astro-ph.IM]. [76] M. Chevallier and D. Polarski, Accelerating Universes with Scaling Dark Matter, International Journal of Modern Physics D10, 213 (2001), arXiv:gr-qc/0009008 [gr-qc]. [77] E.V.Linder,ExploringtheExpansionHistoryoftheUniverse, Phys. Rev. Lett.90, 091301 (2003), arXiv:astro-ph/0208512 [astro-ph]. [78] Euclid Collaboration, M. Knabenhans, J. Stadel, D. Potter, J. Dakin,et al., Euclid preparation: IX. EuclidEmulator2 - power spectrum emulation with massive neutrinos and self- consistentdarkenergyperturbations,Mon.Not.RoyalAstron."},{"citing_arxiv_id":"2510.13752","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effects of primordial magnetic fields on 21 cm multifrequency angular power spectra","primary_cat":"astro-ph.CO","submitted_at":"2025-10-15T16:59:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The paper calculates multifrequency angular power spectra of the 21 cm line for models with primordial magnetic fields of strength 4 nG and spectral indices -2.9 and -2.5, then estimates signal-to-noise ratios for uGMRT, MeerKAT and SKA1-MID.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.15453","ref_index":19,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CosmoGen: A genetic algorithm framework for the exploration of dark energy dynamics","primary_cat":"astro-ph.CO","submitted_at":"2025-09-18T21:50:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"CosmoGen employs evolutionary algorithms for symbolic regression to generate dark energy fluid models that alleviate S8 and H0 tensions, with Bayesian analysis of one model showing tension relief though weaker preference than LambdaCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.03458","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Comparison of Halo Model and Simulation Predictions for Projected-Field Kinematic Sunyaev-Zel'dovich Cross-Correlations","primary_cat":"astro-ph.CO","submitted_at":"2025-09-03T16:33:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Halo model predictions match Websky simulations well for Planck filters but differ by ~20% for Simons Observatory filters, exceeding error bars and consistent with missing higher-order terms in the kSZ signal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.23355","ref_index":60,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"SPT-3G D1: Axion Early Dark Energy with CMB experiments and DESI","primary_cat":"astro-ph.CO","submitted_at":"2025-07-31T09:04:47+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"CMB-only data give f_EDE < 0.07 at 95% CL with no strong AEDE signal, while CMB+DESI yields f_EDE = 0.055^{+0.024}_{-0.047} at 68% CL and lowers Hubble tension to 2.6 sigma.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.13537","ref_index":64,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting $\\Lambda$CDM extensions in light of re-analyzed CMB data","primary_cat":"astro-ph.CO","submitted_at":"2025-06-16T14:26:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Re-analysis with PR4 Planck likelihoods reduces lensing anomaly significance and curvature preference in Lambda CDM extensions while indicating a preference for evolving dark energy consistent with DESI.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14744","ref_index":136,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:18+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"DESI DR2 BAO and full-shape data plus CMB yield ∑m_ν < 0.0642 eV (95% CL) under ΛCDM, in 3σ tension with oscillation lower limits, relaxed to <0.163 eV in w0waCDM.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We use the Cobaya code [131, 132] for cosmologi- cal parameter inference employing Metropolis-Hastings Markov-Chain-Monte-Carlo (MCMC) sampling. Cobaya in turn calls the Boltzmann codes CAMB [133] and CLASS [134, 135], as well as likelihoods for various datasets. The posterior chains are analyzed to derive summary statis- tics and plots using the getdist package [136]. The first set of runs are performed with a ΛCDM model, specified by the first 6 parameters listed in Ta- ble I, complemented with the sum of neutrino masses. The parameter θMC is an approximation to the acoustic angular scale θ∗. This parameter is used only to make steps in the MCMC algorithm, while the actual likeli- hood calculations employ θ∗."},{"citing_arxiv_id":"2503.14743","ref_index":90,"ref_count":1,"confidence":0.98,"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":"method","top_context_polarity":"use_method","context_text":"2012, 027 (2012), arXiv:1201.3654 [astro-ph.CO]. [87] W. Hu and I. Sawicki, Phys. Rev. D 76, 104043 (2007), arXiv:0708.1190 [astro-ph]. [88] W. Fang, W. Hu, and A. Lewis, Phys. Rev. D78, 087303 (2008), arXiv:0808.3125 [astro-ph]. [89] J. Lesgourgues, The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview (2011), arXiv:1104.2932 [astro-ph.IM]. [90] D. Blas, J. Lesgourgues, and T. Tram, J. Cosmology As- tropart. Phys. 1107, 034 (2011), arXiv:1104.2933 [astro- ph.CO]. [91] H. Dembinski and P. O. et al., scikit-hep/iminuit (2020). [92] M. Ishak, J. Pan, R. Calderon, K. Lodha, and oth- ers, arXiv e-prints , arXiv:2411.12026 (2024), 21 arXiv:2411.12026 [astro-ph.CO]. [93] V. Poulin, T. L. Smith, R."},{"citing_arxiv_id":"2410.23348","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observable CMB B-modes from Cosmological Phase Transitions","primary_cat":"astro-ph.CO","submitted_at":"2024-10-30T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Phase transitions in dark sectors can generate CMB B-modes with amplitudes competitive with inflation but peaking at smaller angular scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2306.11053","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid: Constraints on f(R) cosmologies from the spectroscopic and photometric primary probes","primary_cat":"astro-ph.CO","submitted_at":"2023-06-19T16:38:27+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts show Euclid combined probes can constrain log f_R0 at the 1% level for fiducial f_R0=5e-6, distinguishing from LCDM at >3 sigma in optimistic settings.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2304.05202","ref_index":7,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"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":"2211.04492","ref_index":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Hubble Tension and Early Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2022-11-08T19:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.11237","ref_index":122,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"2020 Global reassessment of the neutrino oscillation picture","primary_cat":"hep-ph","submitted_at":"2020-06-19T17:21:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Updated global fit of neutrino oscillation data gives precise measurements of mixing parameters with a 2.5 sigma preference for normal mass ordering.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"2933 [astro-ph.CO] . [120] J. Lesgourgues, \"The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview,\" arXiv:1104.2932 [astro-ph.IM] . [121] P. Astone and G. D'Agostini, \"Inferring the intensity of Poisson processes at the limit of the detector sensitivity (with a case study on gravitational wave burst search),\" Annals Phys. , hep-ex/9909047. [122] G. D'Agostini, \"Confidence limits: What is the problem? Is there the solution?,\" in Workshop on confidence limits, CERN, Geneva, Switzerland, 17-18 Jan 2000: Proceedings , pp. 3-27. 2000. arXiv:hep-ex/0002055 [hep-ex] . [123] G. D'Agostini, Bayesian Reasoning in Data Analysis . WORLD SCIENTIFIC, Jun, 2003. https://doi.org/10.1142%2F5262. [124] S. Gariazzo, \"Constraining power of open likelihoods, made prior-independent,\" Eur."},{"citing_arxiv_id":"2005.05290","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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},{"citing_arxiv_id":"1807.06211","ref_index":259,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. X. Constraints on inflation","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:09+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"we assume instantaneous reheating, which, for a pivot scale of k∗ = 0.05 Mpc−1, corresponds to N∗≈ 57.5, andφ0 = 12.38MPl withφend = 0.59MPl. This leads to definite predictions for (r, ns); namely, (0.0922, 0.971) for p = 4/3, (0.0692, 0.974) for p = 1, and (0.0462, 0.977) for p = 2/3. To constrain this model, we carry out a Bayesian analysis us- ing a modified version of CLASS (Lesgourgues 2011; Blas et al. 2011), which has been adapted to allow for a full parameter ex- ploration, using the aforementioned template. As part of these modifications, special care needs to be taken to ensure that a correct sampling ∆k in wavenumber space is chosen, at two dif- ferent levels in the Boltzmann code: when computing an inter- polation table for the primordial spectrum of scalars and tensors;"},{"citing_arxiv_id":"1104.2933","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation schemes","primary_cat":"astro-ph.CO","submitted_at":"2011-04-14T22:06:43+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"CLASS implements a tunable baryon-photon tight-coupling approximation, a new ultra-relativistic fluid approximation, and a radiation streaming approximation that accounts for reionization, yielding simultaneous gains in speed and precision.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}