Episodic Star Formation. I. Overview and Scatter of the Star-forming Main Sequence

There is mounting evidence for episodic star formation cycles in both high- and low-redshift galaxies. This paper aims to understand the detailed physical processes behind such behaviors and investigate how such an episodic star-forming scenario can explain the scatter in star formation rate (SFR) of star-forming main-sequence (SFMS) galaxies. This is achieved by tracing back in time the history of z = 0 star-forming central galaxies in the TNG100 simulation over the past 7−8 Gyr. As the first paper in this series, we provide an overview of the episodic star formation history. We find that two branches of star formation typically develop during each episode: while one branch happens in heavily metal-enriched gas in the centers of galaxies, a secondary branch starts in lower-metallicity regions at galaxy outskirts where fresh gas first arrives, and gradually progresses to the inner regions of galaxies. Additionally, the temporal variation in the SFR at galaxy outskirts is more significant than that at centers. As a consequence, the metallicities in both gas and young stars exhibit remarkably different distributions between SFR peaks and valleys. The resulting temporal SFR fluctuation within individual galaxies has an average of ∼0.2 dex, while the intrinsic differentiation between (the historical mean of) galaxies is ∼0.15 dex. These two results together can well account for the scatter in SFR of ∼0.25 dex as observed for z = 0 SFMS galaxies.