Quenching, bursting and galaxy shapes: colour transformation as a function of morphology

TL;DR

This study introduces the Star Formation Acceleration parameter to analyze galaxy morphology and star formation changes, revealing that ellipticals quench faster and that massive spirals often undergo bursts linked to interactions.

Contribution

It presents a new methodology using SFA to distinguish bursting and quenching episodes and links these processes to galaxy morphology and interactions.

Findings

Elliptical galaxies have shorter quenching timescales (<1 Gyr) than spirals (≥1 Gyr).

Major mergers influence rapid quenching and morphological transformation.

Massive spirals often show signs of recent interactions and bursts in the green valley.

Abstract

Different mechanisms for quenching star formation in galaxies are commonly invoked in the literature, but the relative impact of each one at different cosmic epochs is still unknown. In particular, the relation between these processes and morphological transformation remains poorly understood. In this work, we measure the effectiveness of changes in star formation rates by analysing a new parameter, the Star Formation Acceleration (SFA), as a function of galaxy morphology. This methodology is capable of identifying both bursting and quenching episodes that occurred in the preceding 300 Myrs. We use morphological classification catalogs based on Deep learning techniques. Our final sample has $\sim$14,200 spirals and $\sim$2,500 ellipticals. We find that elliptical galaxies in the transition region have median shorter quenching timescales ( $\tau$ < 1 Gyr) than spirals ($\tau \geq 1$ Gyr). This result conforms to the scenario in which major mergers and other violent processes play a fundamental role in galaxy evolution for most ellipticals, not only quenching star formation more rapidly but also playing a role in morphological transformation. We also find that $\sim$two thirds of galaxies bursting in the green valley in our sample are massive spirals ($M_\star \geq 10^{11.0}M_\odot$) with signs of disturbance. This is in accordance with the scenario where low mass galaxies are losing their gas in a interaction with a massive galaxy: while the former is quenching, the last is being refueled and going through a burst, showing signs of recent interaction.