Cesam2k20 computes one-dimensional stellar structure and evolution models under the assumption of hydrostatic equilibrium. The code evolves stellar models from pre-main sequence through advanced evolutionary stages using modular numerical schemes and up-to-date microphysics. Cesam2k20 builds on the CESAM (ascl:1010.059) stellar evolution code and incorporates developments from related tools such as ADIPLS (ascl:1109.002) for asteroseismic applications. It includes treatments of processes such as chemical mixing, angular momentum transport, and rotation within a unified framework. Cesam2k20 supports stellar modeling studies in both classical and asteroseismic contexts.

PSLS simulates solar-like oscillators representative of PLATO targets. It includes planetary transits, stochastically-excited oscillations, granulation and activity background components, as well as instrumental systematic errors and random noises representative for PLATO.

SPInS (Stellar Parameters INferred Systematically) provides the age, mass, and radius of a star, among other parameters, from a set of photometric, spectroscopic, interferometric, and/or asteroseismic observational constraints; it also generates error bars and correlations. Derived from AIMS (ascl:1611.014), it relies on a stellar model grid and uses a Bayesian approach to find the PDF of stellar parameters from a set of classical constraints. The heart of SPInS is a MCMC solver coupled with interpolation within a pre-computed stellar model grid. The code can consider priors such as the IMF or SFR and can characterize single stars or coeval stars, such as members of binary systems or of stellar clusters.

CReSyPS (Code Rennais de Synthèse de Populations Stellaires) is a stellar population synthesis code that determines core overshooting amount for Magellanic clouds main sequence stars.