Estimation of the Galaxy Quenching Rate in the Illustris Simulation

Abstract

Quenching is a key topic in exploring the formation and evolution of galaxies. In this work, we study the quenching rate, i.e., the variation in the fraction of quenched galaxies per unit time, of the Illustris-1 simulation. By building the quenched fraction function $f(m,\rho ,t)$ of each snapshot in the simulation, we derive an accurate form of quenching rate as ${\Re }_q=df(m,\rho ,t)/dt$. According to the analytic expression of the quenching rate ${\Re }_q$, we split it into four components: mass quenching, environmental quenching, intrinsic mass quenching and intrinsic environmental quenching. The precise value and evolutions can be given via the formula of ${\Re }_q$. With this method, we analyze the Illustris-1 simulation. We find that quenched galaxies concentrate around $M_{\ast }\simeq 10^{11}{h}^{-1}{M}_{\odot }$ and $\delta +1\simeq 10^{3.5}$ at earlier times, and that the quenching galaxy population slowly shifts to lower stellar mass and lower overdensity regions with time. We also find that mass quenching dominates the quenching process in this simulation, in agreement with some previous analytical models. Intrinsic quenching is the second most important component. Environmental quenching is very weak, because it is possible that the pre- or postprocessing of environments disguises environmental quenching as intrinsic quenching. We find that our method roughly predict the actual quenching rate. It could well predict the actual amount of galaxies quenched by intrinsic quenching. However, it overestimates the amount of mass quenching galaxies and underestimates the amount of environmental quenching. We suggest that the reason is the nonlinearity of the environmental overdensity change and mass growth of the galaxy.

28 pages, 18 figures, 1 table

References in corpus (22)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• Mass and environment as drivers of galaxy evolution in SDSS and zCOSMOS and the origin of the Schechter function
• Star Formation in AEGIS Field Galaxies since z=1.1 : The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-Forming Galaxies
• The hierarchical formation of the brightest cluster galaxies
• 3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since $z=3$
• Properties of galaxies reproduced by a hydrodynamic simulation
• Simba: Cosmological Simulations with Black Hole Growth and Feedback
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time
• The Illustris simulation: the evolving population of black holes across cosmic time
• Structure and star formation in galaxies out to z=3: evidence for surface density dependent evolution and upsizing
• The star formation main sequence and stellar mass assembly of galaxies in the Illustris simulation
• A refined sub-grid model for black hole accretion and AGN feedback in large cosmological simulations
• The First Appearance of the Red Sequence of Galaxies in Proto-Clusters at 2<~z<~3
• Effect of local environment and stellar mass on galaxy quenching and morphology at $0.5<z<2.0$
• The impact of galactic properties and environment on the quenching of central and satellite galaxies: A comparison between SDSS, Illustris and L-Galaxies
• The Rest-Frame Optical Luminosity Function of Cluster Galaxies at z<0.8 and the Assembly of the Cluster Red Sequence
• GMASS Ultradeep Spectroscopy of Galaxies at z~2. III: The emergence of the color bimodality at z~2
• The evolution of the quenching of star formation in cluster galaxies since z $\sim$ 1
• The influence of environment on satellite galaxies in the GAEA semi-analytic model
• The Roles of Mass and Environment in the Quenching of Galaxies. II
• The Roles of Mass and Environment in the Quenching of Galaxies

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