The integrated properties of the CALIFA galaxies: Model-derived galaxy parameters and quenching of star formation

TL;DR

This study analyzes 835 CALIFA galaxies using spectral energy distribution fitting to derive physical parameters, revealing that star formation quenching results from gas deficiency and morphological factors, with limited influence from AGN or environment.

Contribution

It introduces a comprehensive comparison of SED-derived galaxy parameters with IFU spectral modeling, highlighting the advantages of SED fitting for understanding star formation quenching mechanisms.

Findings

Star formation quenching linked to gas deficiency and bulge buildup.

SED-derived SFRs outperform IFU-based estimates.

Morphology strongly correlates with quenching processes.

Abstract

We present a study of the integrated properties of the 835 galaxies in the CALIFA survey. To derive the main physical parameters of the galaxies we have fitted their UV-to-IR spectral energy distributions (SED) with sets of theoretical models using CIGALE. We perform a comparison of the integrated galaxy parameters derived from multi-band SED fitting with those obtained from modelling the Integral Field Unit (IFU) spectra and show the clear advantage of using the SED-derived star formation rates (SFR). A detailed analysis of galaxies in the SFR/Mstar plane as a function of their properties reveals that quenching of star formation is caused by a combination of gas deficiency and the inefficiency of the existing gas to form new stars. Exploring the plausible mechanisms that could produce this effect, we find a strong correlation with galaxy morphology and the build-up of central bulge. On the other hand, the presence of AGN and/or a stellar bar, as well as the local environment have only temporal effects on the current star formation, a result also consistent with their model-derived star formation histories.