Radial Profiles of $\Sigma_{\ast}$, $\Sigma_{\rm SFR}$, Gas Metallicity and Their Correlations Across the Galactic Mass-Size Plane

TL;DR

This study examines how the internal properties and radial profiles of star-forming galaxies vary with galaxy size and mass, revealing that compact galaxies have distinct metallicity, star formation, and structural characteristics compared to extended ones.

Contribution

It provides a detailed comparison of radial profiles of stellar mass, SFR, and metallicity between compact and extended galaxies at fixed stellar mass, highlighting the role of galaxy size and angular momentum.

Findings

Compact galaxies have higher central sSFR and metallicity.

Steeper metallicity gradients are found in extended galaxies.

Radial SFR profiles depend on factors beyond mass and surface density.

Abstract

We analyzed the global and resolved properties of approximately 1,240 nearby star-forming galaxies from the MaNGA survey, comparing compact and extended galaxies -- those with smaller and larger radii ($R_{\rm e}$), respectively -- at a fixed stellar mass ($M_{\ast}$). Compact galaxies typically exhibit lower HI gas fractions, higher dust extinction, higher metallicity, greater mass concentration, and lower angular momentum on a global scale. Radial profiles of stellar mass surface density ($\Sigma_{\ast}$) and star formation rate surface density ($\Sigma_{\rm SFR}$), as functions of the effective radius ($R/$$R_{\rm e}$), reveal that compact galaxies display steeper gradients and higher values, resulting in elevated specific star formation rates (sSFR) in their inner regions compared to their outskirts. At a given $\Sigma_{\ast}$, compact galaxies have higher sSFR than extended galaxies, particularly in low-mass galaxies (log($M_{\ast}$/$M_{\odot}$)$\,\leq\,$10$^{10}$). Additionally, their metallicity profiles differ significantly: extended galaxies have steeper metallicity gradients, while compact galaxies exhibit flatter slopes and higher metallicity at a given $R/$$R_{\rm e}$. After accounting for the dependence of metallicity on $M_{\ast}$ and $\Sigma_{\ast}$, no further correlation with SFR is observed. The combination of higher sSFR and potentially higher star formation efficiency in compact galaxies suggests that their central gas is being rapidly consumed, leading to older stellar populations, as indicated by D$_{n}$(4000) and EW(H$\delta_A$), and resulting in faster central growth. Our results reveal that radial SFR profiles cannot be fully determined by $M_{\ast}$ and $\Sigma_{\ast}$ alone; other factors, such as galaxy size or angular momentum, must be considered to fully understand the observed trends.