Effects of environment on stellar metallicity profiles of late-type galaxies in the CALIFA survey

TL;DR

This study investigates how environment influences the metallicity profiles of late-type galaxies, revealing that group galaxies are more metal-rich and exhibit different metallicity gradient patterns compared to field galaxies, indicating distinct evolutionary paths.

Contribution

It provides a comparative analysis of metallicity profiles in late-type galaxies across different environments using CALIFA survey data, highlighting environmental effects on galaxy evolution.

Findings

Group galaxies are systematically more metallic than field galaxies.

Field galaxies show negative metallicity gradients in inner regions, flatter at larger radii.

Group galaxies tend to have flat inner metallicity profiles and negative outer gradients.

Abstract

We explore the effects of environment in the evolution of late-type galaxies by studying the radial profiles of light- and mass-weighted metallicities of galaxies in two discrete environments: field and groups. We use a sample of 167 late-type galaxies, with stellar masses $9\le \log(M_{\star}/M_{\odot}) \le 12$, drawn from the CALIFA survey. We make a study of the metallicity of galaxies in these two environments which includes the comparison of the metallicity as a function of the radius, at a characteristic scale, and as a function of a the stellar mass surface density. We find significant differences between group and field late-type galaxies in terms of their metallicity, in the sense that group galaxies are systematically more metallic than their field counterparts. We find that field galaxies have, in general, metallicity profiles that show a negative gradient in their inner regions, and a shallower profile at larger radii. This contrasts with the metallicity profiles of galaxies in groups, which tend to be flat in the inner regions, and to have a negative gradient in the outer parts. Regarding the metallicity at the characteristic radius of the luminosity profiles, we consistently find that it is higher for group galaxies irrespective of galaxy mass. At fixed local stellar surface mass density, group galaxies are again more metallic, also the dependence of metallicity on surface density is less important for group galaxies. The evidence of a clear difference on the metallicity of group and field galaxies, as a function of mass, spatial scale, and local stellar mass density, are indicative of the different evolutionary paths that galaxies in groups and in the field have followed. We discuss possible implications of the observed differences.