Efficient Computation of Cosmic Microwave Background Anisotropies in Closed Friedmann-Robertson-Walker Models

By A. Lewis, A. Challinor, A. Lasenby. 2000

441 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2dff4f4e13cdd184cb4483df46f3b5c06fa22824

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Citations in the corpus

Dark energy or modified gravity? An effective field theory approach (2012, methodology): “Furthermore, we envisage our equations being used in modified versions of software such as CAMB [30], which uses synchronous gauge.”
Cosmology with massive neutrinos I: towards a realistic modeling of the relation between matter, haloes and galaxies (2013, methodology): “We also find that the Tinker fitting formula reproduces reasonably well our results, in terms of the bias on large 8In our case we incorporate the baryons effects into the CDM particles when generating the initial conditions by setting: Tcdm(k) = [Ωcdm Tcdm(k) + Ωb Tb(k)]/(Ωcdm + Ωb), where Tcdm(k) ”
Cosmological parameters derived from the final Planck data release (PR4) (2023, methodology): “The model for the CMB was computed by numerically solving the background and perturbation equations for a speciﬁc cosmological model using CAMB (Lewis et al. 2000; Howlett et al. 2012) 6 .”
THE 1% CONCORDANCE HUBBLE CONSTANT (2014, methodology): “We acknowledge use of the HEALPix (Gorski et al. 2005) and CAMB (Lewis et al. 2000) packages.”
Alleviating the H0 and σ8 anomalies with a decaying dark matter model (2019, methodology): “To investigate this DDM model, we use a modified version of the publicly available Boltzmann code CAMB [55].”
Lyman-alpha forests cool warm dark matter (2015, methodology): “, each set of parameters), the initial matter power spectrum is generated using the CAMB software(5) [11] down to z = 30.”
Constraint on neutrino masses from SDSS-III/BOSS Lyα forest and other cosmological probes (2014, methodology): “The simulations were run using CAMB1 [34] to compute the transfer functions and linear power spectra at z = 30, then 2LPT2 (second-order Lagrangian Pertur1http://camb.”
A tale of two modes: neutrino free-streaming in the early universe (2017, methodology): “7) numerically along with perturbation equations for other standard cosmological components such as baryonic matter, photons, and cold dark matter using a version of the code CAMB modified for the purposes of this study [95, 96].”
Constraints from Ly-α forests on non-thermal dark matter including resonantly-produced sterile neutrinos (2017, methodology): “We solve the Boltzmann equations in the expanding Universe numerically with the CAMB7 [58] and CLASS8 [59] softwares and compute the linear power spectrum of matter density fluctuations at z = 30.”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “6 eV, has been computed with the software camb [743].”
Robust forecasts on fundamental physics from the foreground-obscured, gravitationally-lensed CMB polarization (2015, methodology): “(2.21), with the following replacement (Cφφ` ) 2 Cφφ` +N φφ ` → Cφφ, zmax` , (2.26) where Cφφ, zmax` is the power spectrum of the lensing potential including contributions from z ≤ zmax only (calculated using a modified version of CAMB [66]).”
DeepCMB: Lensing Reconstruction of the Cosmic Microwave Background with Deep Neural Networks (2018, methodology): “These simulations are created given the E and κ power spectra generated based on Planck 2013 best-fit ΛCDM cosmology: Ωbh2 = 0.0222, ΩCDMh2 = 0.1185, As = 2.21 ×10−9, ns = 0.9624, τ = 0.0943, H0 = 67.94, using CAMB (Lewis et al., 2000) and HEALPix1 and lensed with the quicklens2 package.”