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.
Bertschinger, arXiv:astro-ph/9506070
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abstract
COSMICS is a package of fortran programs useful for computing transfer functions and microwave background anisotropy for cosmological models, and for generating gaussian random initial conditions for nonlinear structure formation simulations of such models. Four programs are provided: {\bf linger\_con} and {\bf linger\_syn} integrate the linearized equations of general relativity, matter, and radiation in conformal Newtonian and synchronous gauge, respectively; {\bf deltat} integrates the photon transfer functions computed by the linger codes to produce photon anisotropy power spectra; and {\bf grafic} tabulates normalized matter power spectra and produces constrained or unconstrained samples of the matter density field. Version 1.0 of COSMICS is available at http://arcturus.mit.edu/cosmics/ . The current release gives fortran-77 programs that run on workstations and vectorized supercomputers. Unix makefiles are included that make it simple to build and test the package. A future release will include portable parallel versions of the linger codes using standard message-passing libraries.
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astro-ph.CO 2representative citing papers
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.
citing papers explorer
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The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation schemes
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.
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The Hubble Tension and Early Dark Energy
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.