The P\'egase.3 code of spectrochemical evolution of galaxies: documentation and complements

TL;DR

Pégase.3 is a comprehensive Fortran 95 code that models the spectral and chemical evolution of galaxies from ultraviolet to submillimeter wavelengths, incorporating dust emission, nebular emission, and complex evolutionary scenarios.

Contribution

It introduces advanced modeling of dust emission, nebular lines with metallicity effects, and supports complex galaxy evolution scenarios, improving upon previous versions.

Findings

Enhanced dust emission modeling with stochastic heating.

Updated nebular emission calculations considering metallicity.

Supports complex, multi-episode galaxy evolution scenarios.

Abstract

P\'egase.3 is a Fortran 95 code modeling the spectral evolution of galaxies from the far-ultraviolet to submillimeter wavelengths. It also follows the chemical evolution of their stars, gas and dust. For a given scenario (a set of parameters defining the history of mass assembly, the star formation law, the initial mass function...), P\'egase.3 consistently computes the following: * the star formation, infall, outflow and supernova rates from 0 to 20 Gyr; * the stellar metallicity, the abundances of main elements in the gas and the composition of dust; * the unattenuated stellar spectral energy distribution (SED); * the nebular SED, using nebular continua and emission lines precomputed with code Cloudy (Ferland et al. 2017); * the attenuation in star-forming clouds and the diffuse interstellar medium, by absorption and scattering on dust grains, of the stellar and nebular SEDs. For this, the code uses grids of the transmittance for spiral and spheroidal galaxies. We precomputed these grids through Monte Carlo simulations of radiative transfer based on the method of virtual interactions; * the re-emission by grains of the light they absorbed, taking into account stochastic heating. The main innovation compared to P\'egase.2 is the modeling of dust emission and its evolution. The computation of nebular emission has also been entirely upgraded to take into account metallicity effects and infrared lines. Other major differences are that complex scenarios of evolution (derived for instance from cosmological simulations), with several episodes of star formation, infall or outflow, may now be implemented, and that the detailed evolution of the most important elements -- not only the overall metallicity -- is followed.