Numerical simulations across 10 cosmologies reveal stronger perpendicular void-surface halo alignments in models with more dynamic dark energy, quantified by fitted parameter d_t that follows a bilinear relation with w and wa.
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The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview
Mixed citation behavior. Most common role is method (62%).
64
Pith papers citing it
Method
62% of classified citations
abstract
The Cosmic Linear Anisotropy Solving System (CLASS) is a new accurate Boltzmann code, designed to offer a more user-friendly and flexible coding environment to cosmologists. CLASS is very structured, easy to modify, and offers a rigorous way to control the accuracy of output quantities. It is also incidentally a bit faster than other codes. In this overview, we present the general principles of CLASS and its basic structure. We insist on the friendliness and flexibility aspects, while accuracy, physical approximations and performances are discussed in a series of companion papers.
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method 16
background 9
dataset 1
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representative citing papers
Computes anisotropic CMB spectral distortion power spectra from photon-dark photon conversions, finding that mass controls multipole shape and mixing sets amplitude, then places Planck limits on the minimal model.
Any unified early and late dark energy scenario with a single tracking scalar field requires a potential with three distinct slopes arranged in a steep-steeper-shallow hierarchy.
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.
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.
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.
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.
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.
Cobaya is a modular Bayesian analysis code that exploits model interdependencies via automatic caching and a novel parameter-blocking algorithm to minimize sampling cost.
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.
Composite dark matter from a keV-MeV confining phase transition generates curvature perturbations constrained by CMB anisotropies and Lyman-alpha forest data, offering a testable scenario even without visible sector couplings.
LLM embeddings condition a generative transformer to enable faster convergence, better performance, and generalization to unseen LHC processes using a single model.
ACG models embed the observationally preferred phantom-crossing dark energy behavior inside a consistent Horndeski Lagrangian and achieve data fits of similar quality to w0waCDM while being narrowed by perturbative probes.
Manticore-Deep uses tiled Bayesian field-level inference on SDSS and BOSS data to produce posterior ensembles of 3D cosmic fields that are consistent with LCDM and validated by 7.4σ CMB lensing and 3.5σ kSZ detections.
CMBolic supplies analytic emulators for CMB lensing spectra achieving 0.27-0.32% mean fractional error, validated against CLASS on ACT DR6 and Planck lensing data.
A geometric landscape of mixed states for cosmological perturbations unifies decoherence models and derives non-linearity bounds that rule out decohered thermal states and limit amplitude-diagonal models to under 70 e-folds of inflation.
Calibrates a one-parameter semi-analytic damping model for oscillatory primordial power spectrum features using N-body simulations and validates sub-percent accuracy via GPR emulation when modulation frequency is high enough.
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.
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.
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.
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.
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.
Estimators from squeezed bispectrum and collapsed trispectrum recover unbiased small-scale matter power spectrum covariance at the percent level using 25 Quijote simulations.
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.
citing papers explorer
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Late-Time Cosmology and Structure Formation in Quadratic $f(Q)$ Gravity
Quadratic f(Q) gravity adds an H^4 term to the Friedmann equation and introduces a time-dependent G_eff that suppresses linear growth and halo abundance, offering a modified-gravity route to easing the S8 tension.