A$^3$COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time

TL;DR

This study investigates the dust content and evolution of massive quiescent galaxies from redshift 0.5 to 3, revealing rapid ISM depletion post-quenching and providing new constraints on their cold gas and dust properties over cosmic time.

Contribution

It provides the first comprehensive analysis of dust evolution in massive quiescent galaxies across a wide redshift range using stacking techniques and spectral energy distribution fitting.

Findings

Most QGs quenched around z~1.3, post peak cosmic star formation.

High-z QGs are recently quenched, low-z QGs have long been quiescent.

QGs lose >70% of cold ISM within 600 Myr after quenching.

Abstract

We study the dust content of massive ($\log(M_*/M_{\odot})\geq10.8$) quiescent galaxies (QGs) at redshifts $z=0.5-3$ to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. We used a robust sample of 458 colour-selected QGs covered by the A$^3$COSMOS+A$^3$GOODSS database to perform a stacking analysis in the $uv$ domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Most QGs in our sample quenched around a redshift of $z\sim1.3$, following the peak of cosmic star formation. The majority of QGs observed at $z>1$ are recently quenched (i.e. quenched for no longer than 500 Myr), whereas the majority of QGs observed at $z<1$ have already been quenched for a significant amount of time ($\gtrsim1$ Gyr). This implies that high-redshift galaxies ($z\gtrsim2$) are ideal for studying the mechanisms of quenching and its effects on the ISM, while lower-redshift galaxies are more suitable for studying the long-term effects of the QG environment on their ISM. We obtain upper limits on the dust mass fraction of the QG population that indicate a lower dust content than what was found by earlier stacking studies, and significantly lower (by a factor of $\sim2-6$) than that of normal star-forming galaxies. We also place constraints on the initial gas fraction right after quenching. We find that within the first $\sim600$ Myr after quenching, QGs already lose on average $\gtrsim70\%$ of their cold ISM. Our findings support a gas consumption or removal scenario acting on short timescales.