The stellar mass function of quiescent and star-forming galaxies and its dependence on morphology in COSMOS-Web
Authors
Marko Shuntov
Olivier Ilbert
Claudia del P. Lagos
Sune Toft
Francesco Valentino
Wilfried Mercier
Hollis B. Akins
Nguyen Binh
Malte Brinch
Caitlin M. Casey
Maximilien Franco
Fabrizio Gentile
Ghassem Gozaliasl
Aryana Haghjoo
Santosh Harish
Michaela Hirschmann
Marc Huertas-Company
Shuowen Jin
Jeyhan S. Kartaltepe
Anton M. Koekemoer
Clotilde Laigle
Joseph S. W. Lewis
Georgios E. Magdis
Henry Joy McCracken
Bahram Mobasher
Thibaud Moutard
Pascal A. Oesch
Louise Paquereau
Alvio Renzini
Michael R. Rich
David B. Sanders
Greta Toni
Laurence Tresse
Andrea Weibel
John R. Weaver
Lilan Yang
Abstract
We study the stellar mass function (SMF) of quiescent and star-forming galaxies and its dependence on morphology in 10 redshift bins at $0.20.6$) dominate the quiescent SMF at ${\rm log}(M_{\star}/{\rm M_{\odot}})>10$ at all redshifts, while disks ($B/T<0.2$) dominate at ${\rm log}(M_{\star}/{\rm M_{\odot}})<9$. However, most bulge-dominated galaxies are star-forming, with their fraction increasing with redshift and decreasing mass, consistent with being progenitors of quiescent bulges. We find evidence for environmental quenching onset at $z\sim3$ from the upturn in the quiescent SMF at ${\rm log}(M_{\star}/{\rm M_{\odot}})<9.5$, contributed by disk-dominated galaxies consistent with satellite quenching that retains disk morphologies. Number densities of ${\rm log}(M_{\star}/{\rm M_{\odot}})>10$ quiescent galaxies are lower than recent literature by $0.1-0.7$ dex, but agree well with simulations at $23$, simulations increasingly underpredict observations. Finally, we build an empirical model describing galaxy number density evolution by parametrizing quenching rates, baryon conversion efficiency, and bulge formation. Our model supports a scenario where star-forming galaxies grow central bulges before quenching in massive halos.
