Abstract

We study the global star-formation rate (SFR) vs. stellar mass (M-*) correlation, and the spatially-resolved SFR surface density (Sigma(SFR)) vs. stellar mass surface density (Sigma(*)) correlation, in a sample of similar to 2,000 galaxies from the MaNGA MPL-5 survey. We classify galaxies and spatially-resolved areas into star-forming and retired according to their ionization processes. We confirm the existence of a Star-Forming Main Sequence (SFMS) for galaxies and spatially-resolved areas, and show that they have the same nature, with the global as a consequence of the local one. The latter presents a bend below a limit Sigma(*) value, approximate to 3x10(7) M(circle dot)kpc(-2), which is not physical. Using only star-forming areas (SFAs) above this limit, a slope and a scatter of approximate to 1 and approximate to 0.27 dex are determined. The retired galaxies/areas strongly segregate from their respective SFMS's, by similar to-1.5 dex on average. We explore how the global/local SFMS's depend on galaxy morphology, finding that for star-forming galaxies and SFAs, there is a trend to lower values of star-formation activity with earlier morphological types, which is more pronounced for the local SFMS. The morphology not only affects the global SFR due to the diminish of SFAs with earlier types, but also affects the local SF process. Our results suggest that the local SF at all radii is established by some universal mechanism partially modulated by morphology. Morphology seems to be connected to the slow aging and sharp decline of the SF process, and on its own it may depend on other properties as the environment.