Different influence of gas accretion on the evolution of star-forming and non-star-forming galaxies

Abstract

Using integral field spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory survey, we investigate the spatially resolved properties and empirical relations of a star-forming galaxy and a non-star-forming galaxy hosting counter-rotating stellar disks (CRDs). The DESI $g, r, z$ color images reveal no evidence of merger remnants in either galaxy, suggesting that gas accretion fuels the formation of CRDs. Based on the visible counter-rotation in the stellar velocity field, we can fit a spatial boundary to distinguish the inner and outer regions dominated by two stellar disks in each galaxy. In the inner region of the star-forming CRDs, stars are co-rotating with ionized gas, and the stellar population is younger. Comparison of the star-forming main sequence relations between the inner and outer regions reveals enhanced star formation in the inner region. Given the abundant pre-existing gas in the star-forming galaxy, collisions between pre-existing and external gas efficiently consume angular momentum, triggering star formation in the inner region. Conversely, in the outer region of the non-star-forming CRDs, stars are co-rotating with ionized gas, and the stellar population is younger. Comparison of the stellar mass-metallicity relations between the inner and outer regions indicates enriched gas-phase metallicity in the outer region. Considering the less abundant pre-existing gas in the non-star-forming galaxy, external gas could preserve angular momentum, fueling star formation in the outer region. Overall, gas accretion exhibits different influence on the evolution of star-forming and non-star-forming galaxies.