ChempyMulti is an update to Chempy (ascl:1702.011) and provides yield table scoring and multi-star Bayesian inference. This replaces the ChempyScoring package in Chempy. Chempy is a flexible one-zone open-box chemical evolution model, incorporating abundance fitting and stellar feedback calculations. It includes routines for parameter optimization for simulations and observational data and yield table scoring.

RascalC quickly estimates covariance matrices from two- or three-point galaxy correlation functions. Given an input set of random particle locations and a two-point correlation function (or input set of galaxy positions), RascalC produces an estimate of the associated covariance for a given binning strategy, with non-Gaussianities approximated by a ‘shot-noise-rescaling’ parameter. For the 2PCF, the rescaling parameter can be calibrated by dividing the particles into jackknife regions and comparing sample to theoretical jackknife covariance. RascalC can also be used to compute Legendre-binned covariances and cross-covariances between different two-point correlation functions.

HADES analyzse dust levels in simulated CMB galactic dust maps with realistic experimental noise and lensing configurations. It allows detection of dust via its anisotropy properties in CMB B-modes. It also includes techniques for computing null-tests and a rudimentary technique for dedusting.

HIPSTER (HIgh-k Power Spectrum EstimatoR) computes small-scale power spectra and isotropic bispectra for cosmological simulations and galaxy surveys of arbitrary shape. The code computes the Legendre multipoles of the power spectrum, P_ℓ(k), or bispectrum B_ℓ(k₁,k₂), by computing weighted pair counts over the simulation box or survey, truncated at some maximum radius. The code can be run either in 'aperiodic' or 'periodic' mode for galaxy surveys or cosmological simulations respectively. HIPSTER also supports weighted spectra, for example when tracer particles are weighted by their mass in a multi-species simulation. Generalization to anisotropic bispectra is straightforward (and requires no additional computing time) and can be added on request.

encore (Efficient N-point Correlator Estimation) estimates the isotropic NPCF multipoles for an arbitrary survey geometry in O(N²) time, with optional GPU support. The code features support for the isotropic 2PCF, 3PCF, 4PCF, 5PCF and 6PCF, with the option to subtract the Gaussian 4PCF contributions at the estimator level. For the 4PCF, 5PCF and 6PCF algorithms, the runtime is dominated by sorting the spherical harmonics into bins, which has complexity O(N_galaxy x N_bins³ x N_ell⁵) [4PCF], O(N_galaxy x N_bins⁴ x N_ell⁸) [5PCF] or O(N_galaxy x N_bins⁵ x N_ell¹¹) [6PCF]. The higher-point functions are slow to compute unless N_bins and N_ell are small.

Kepler's Goat Herd solves Kepler's equation using contour integration to solve the "geometric goat problem". The C++ code implements a variety of solution: 1.) Newton-Raphson: The quadratic Newton-Raphson root finder; 2.) Danby: The quartic root; 3.) Series: An elliptical series method; and 4.) Contour: A new method based on contour integration. Given an array of mean anomalies, an eccentricity and a desired precision, the code estimates the eccentric anomaly using each method. The accuracy of each approach is increased until the desired precision is reached, and timing is performed using the C++ chrono package.

Spectra-Without-Windows (formerly called BOSS-Without-Windows) analyzes Baryon Oscillation Spectroscopic Survey (BOSS) DR12 data using quadratic and cubic estimators. It contains analysis codes to estimate unwindowed power spectra and unwindowed bispectra. It also supplies the raw power and bispectrum spectrum measurements of BOSS and 999 Patchy simulations, and contains a utility function to generate the background number density, n(r) from the survey mask and n(z) distribution. This code has been replaced by the newer and more powerful 3D polyspectrum code PolyBin3D (ascl:2404.006).

PolyBin estimates the binned power spectrum, bispectrum, and trispectrum for full-sky HEALPix maps such as the CMB. This can include both spin-0 and spin-2 fields, such as the CMB temperature and polarization, or galaxy positions and galaxy shear. Alternatively, one can use only scalar maps. For each statistic, two estimators are available: the standard (ideal) estimators, which do not take into account the mask, and window-deconvolved estimators. For the second case, a Fisher matrix must be computed; this depends on binning and the mask, but does not need to be recomputed for each new simulation. PolyBin can compute both the parity-even and parity-odd components, accounting for any leakage between the two, for the bispectrum and trispectrum.

reMASTERed reconstructs ensemble-averaged pseudo-$C_\ell$ to effectively exact precision, with significant improvements over traditional estimators for cases where the map and mask are correlated. The code can compute the results given an arbitrary map and mask; it can also compute the results in the ensemble average for certain types of threshold masks.

PolyBin3D estimates the binned power spectrum and bispectrum for 3D fields such as the distributions of matter and galaxies. For each statistic, two estimators are available: the standard (ideal) estimators, which do not take into account the mask, and window-deconvolved estimators. In the second case, the computation of a Fisher matrix is required; this depends on binning and the mask, but does not need to be recomputed for each new simulation. PolyBin3D supports GPU acceleration using JAX. It is a sister code to PolyBin (ascl:2307.020), which computes the polyspectra of data on the two-sphere, and is a modern reimplementation of the former Spectra-Without-Windows (ascl:2108.011) code.

OneLoopBispectrum computes the one-loop bispectrum of galaxies in redshift space. It computes and simplifies the bispectrum kernels using Mathematica; this is cosmology-independent. The code also computes the full and flattened bispectrum templates, given the pre-computed integration kernels. OneLoopBispectrum uses Mathematica to read in and combine the bispectrum templates, and Python to interpolate and extract the one-loop bispectrum.

CLASS-PT modifies the CLASS (ascl:1106.020) code to compute the non-linear power spectra of dark matter and biased tracers in one-loop cosmological perturbation theory, for both Gaussian and non-Gaussian initial conditions. CLASS-PT can be interfaced with the MCMC sampler MontePython (ascl:1805.027) using the (new and improved) custom-built likelihoods found here.