Star Formation Quenching in Green Valley Galaxies at $0.5\lesssim z\lesssim1.0$ and Constraints with Galaxy Morphologies

TL;DR

This study investigates how galaxy morphology influences star formation quenching timescales at intermediate redshifts ($z extasciitilde0.5-1$), revealing that different morphologies have distinct quenching durations and mechanisms.

Contribution

It provides the first detailed analysis of star formation quenching timescales across various galaxy morphologies at $z extasciitilde0.5-1$, highlighting the role of galaxy interactions over secular evolution.

Findings

Disks have quenching timescales 60% to 5 times longer than spheroidal, irregular, or merger galaxies.

Barred galaxies exhibit the slowest transition through the green valley.

Interaction-driven processes contribute more to rapid quenching at these redshifts.

Abstract

We calculate the star formation quenching timescales in green valley galaxies at intermediate redshifts ($z\sim0.5-1$) using stacked zCOSMOS spectra of different galaxy morphological types: spheroidal, disk-like, irregular and merger, dividing disk-like galaxies further into unbarred, weakly-barred and strongly-barred, assuming a simple exponentially-decaying star formation history model and based on the H$_{\delta}$ absorption feature and the $4000$ \AA ~break. We find that different morphological types present different star formation quenching timescales, reinforcing the idea that the galaxy morphology is strongly correlated with the physical processes responsible for quenching star formation. Our quantification of the star formation quenching timescale indicates that disks have typical timescales $60\%$ to 5 times longer than that of galaxies presenting spheroidal, irregular or merger morphologies. Barred galaxies in particular present the slowest transition timescales through the green valley. This suggests that although secular evolution may ultimately lead to gas exhaustion in the host galaxy via bar-induced gas inflows that trigger star formation activity, secular agents are not major contributors in the rapid quenching of galaxies at these redshifts. Galaxy interaction, associated with the elliptical, irregular and merger morphologies contribute, to a more significant degree, to the fast transition through the green valley at these redshifts. In the light of previous works suggesting that both secular and merger processes are responsible for the star formation quenching at low redshifts, our results provide an explanation to the recent findings that star formation quenching happened at a faster pace at $z\sim0.8$.