Modelling galaxy spectra in presence of interstellar dust-III. From nearby galaxies to the distant Universe

TL;DR

This paper develops advanced spectrophotometric galaxy models that incorporate dust effects, covering a range of morphologies from spherical to disc galaxies, and tests their ability to reproduce observed galaxy spectra across different redshifts.

Contribution

It introduces a comprehensive galaxy modeling approach that accounts for dust, molecular clouds, and stellar populations, improving upon standard EPS techniques for diverse galaxy types.

Findings

Models successfully reproduce observed SEDs of local galaxies.

Incorporating dust significantly affects spectral energy distributions.

Models can be applied to galaxies across different redshifts.

Abstract

Improving upon the standard evolutionary population synthesis (EPS) technique, we present spectrophotometric models of galaxies whose morphology goes from spherical structures to discs, properly accounting for the effect of dust in the interstellar medium (ISM). These models enclose three main physical components: the diffuse ISM composed by gas and dust, the complexes of molecular clouds (MCs) where active star formation occurs and the stars of any age and chemical composition. These models are based on robust evolutionary chemical models that provide the total amount of gas and stars present at any age and that are adjusted in order to match the gross properties of galaxies of different morphological type. We have employed the results for the properties of the ISM presented in Piovan, Tantalo & Chiosi (2006a) and the single stellar populations calculated by Cassar\`a et al. (2013) to derive the spectral energy distributions (SEDs) of galaxies going from pure bulge to discs passing through a number of composite systems with different combinations of the two components. The first part of the paper is devoted to recall the technical details of the method and the basic relations driving the interaction between the physical components of the galaxy. Then, the main parameters are examined and their effects on the spectral energy distribution of three prototype galaxies are highlighted. We conclude analyzing the capability of our galaxy models in reproducing the SEDs of real galaxies in the Local Universe and as a function of redshift.