The effects of environment on galaxies' dynamical structures: From simulations to observations

Abstract

We studied the effects of cluster environments on galactic structures by using the TNG50 cosmological simulation and observed galaxies in the Fornax cluster. We focused on galaxies with stellar masses of $10^{8-12}{M}_{\odot }$ at z=0 that reside in Fornax-like clusters with total masses of $M_{200c}=10^{13.4-14.3}{M}_{\odot }$. We characterized the stellar structures by decomposing each galaxy into a dynamically cold disk and a hot non-disk component, and studied the evolution of both the stellar and gaseous constituents. In TNG50, we find that the cold gas is quickly removed when a galaxy falls into a Fornax-mass cluster. About 87\% of the galaxies have lost $80\%$ of their star-forming gas at 4 billion years after infall, with the remaining gas concentrating in the inner regions of the galaxy. The radius of the star-forming gaseous disk decreases to half its original size at 4 billion years after infall for 66\% of the galaxies. As a result, star formation in the extended dynamically cold disk sharply decreases, even though a low level of SF persists at the center for a few additional gigayears. This leads to a tight correlation between the average stellar age in the dynamically cold disk and the infall time of galaxies. Furthermore, the luminosity fraction of the dynamically cold disk in ancient infallers is only about 1/3 of that in recent infallers, controlling for galaxy stellar mass. This quantitatively agrees with what is observed in early-type galaxies in the Fornax cluster. Gas removal stops the possible growth of the disk, with gas removed earlier in galaxies that fell in earlier, and hence the cold-disk fraction is correlated with the infall time. The stellar disk can be significantly disrupted by tidal forces after infall, through a long-term process that enhances the difference among cluster galaxies with different infall times.

arXiv commentAccepted to A&A, 16 pages, 12 figures

References in corpus (58)

• Planck 2013 results. XVI. Cosmological parameters
• Populating a cluster of galaxies - I. Results at z=0
• E pur si muove: Galiliean-invariant cosmological hydrodynamical simulations on a moving mesh
• Mass and environment as drivers of galaxy evolution in SDSS and zCOSMOS and the origin of the Schechter function
• Simulating Galaxy Formation with the IllustrisTNG Model
• First results from the IllustrisTNG simulations: matter and galaxy clustering
• First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies
• First results from the IllustrisTNG simulations: the galaxy color bimodality
• First results from the IllustrisTNG simulations: A tale of two elements -- chemical evolution of magnesium and europium
• Simulating galaxy formation with black hole driven thermal and kinetic feedback
• The Atlas3D project -- I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria
• Evolution since z = 0.5 of the Morphology-Density relation for Clusters of Galaxies
• First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback
• First Results from the TNG50 Simulation: The evolution of stellar and gaseous disks across cosmic time
• The Origin of Star Formation Gradients in Rich Galaxy Clusters
• The 2dF Galaxy Redshift Survey: The environmental dependence of galaxy star formation rates near clusters
• Ram Pressure Stripping of Spiral Galaxies in Clusters
• Relationship between environment and the broad-band optical properties of galaxies in the SDSS
• Galaxy evolution in groups and clusters: satellite star formation histories and quenching timescales in a hierarchical Universe
• The Atlas3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation
• Mass estimation in the outer regions of galaxy clusters
• Strangulation in Galaxy Groups
• Substructure and dynamics of the Fornax Cluster
• Phase-space Analysis in the Group and Cluster environment: Time since Infall and Tidal Mass Loss
• The effect of ram pressure on the star formation, mass distribution and morphology of galaxies
• On the influence of ram-pressure stripping on the star formation of simulated spiral galaxies
• Enhanced star formation in both disks and ram pressure stripped tails of GASP jellyfish galaxies
• Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing
• Quenched fractions in the IllustrisTNG simulations: comparison with observations and other theoretical models
• Effect of environment on galaxies mass-size distribution: unveiling the transition from outside-in to inside-out evolution
• Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context
• The Atlas3D project - XXIV. The intrinsic shape distribution of early-type galaxies
• Kinematics of tidal tails in interacting galaxies: Tidal Dwarf Galaxies and projection effects
• Atomic hydrogen in IllustrisTNG galaxies: the impact of environment parallelled with local 21-cm surveys
• Orbital decomposition of CALIFA spiral galaxies
• MUSE observations of M87: radial gradients for the stellar initial-mass function and the abundance of Sodium
• The abundance of satellites around Milky Way- and M31-like galaxies with the TNG50 simulation: a matter of diversity
• Distribution of Slow and Fast Rotators in the Fornax Cluster
• The fate of disk galaxies in IllustrisTNG clusters
• The relationship between fine galaxy stellar morphology and star formation activity in cosmological simulations: a deep learning view
• Slow-then-rapid quenching as traced by tentative evidence for enhanced metallicities of cluster galaxies at z~0.2 in the slow quenching phase
• WALLABY Pilot Survey: the diversity of ram pressure stripping of the galactic HI gas in the Hydra Cluster
• The cumulative star-formation histories of dwarf galaxies with TNG50. I: Environment-driven diversity and connection to quenching
• Jellyfish galaxies with the IllustrisTNG simulations -- When, where, and for how long does ram pressure stripping of cold gas occur?
• Mass of the dynamically hot inner stellar halo predicts the ancient accreted stellar mass
• Satellites of Milky Way- and M31-like galaxies with TNG50: quenched fractions, gas content, and star formation histories
• Simulated Bars May Be Shorter But Are Not Slower Than Observed: TNG50 vs. MaNGA
• A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations
• Molecular hydrogen in IllustrisTNG galaxies: carefully comparing signatures of environment with local CO & SFR data
• The Kinematics and Dark Matter Fractions of TNG50 Galaxies at z=2 from an Observational Perspective
• Global HI asymmetries in IllustrisTNG: a diversity of physical processes disturb the cold gas in galaxies
• A jolt to the system: ram pressure on low-mass galaxies in simulations of the Local Group
• The Fornax3D project: Environmental effects on the assembly of dynamically cold disks in Fornax cluster galaxies
• Quantifying the stellar ages of dynamically separated bulges and disks of CALIFA spiral galaxies
• When the Well Runs Dry: Modeling Environmental Quenching of High-mass Satellites in Massive Clusters at \boldmath$z\gtrsim 1$
• Characteristic mass in galaxy quenching: environmental versus internal effects
• The Local Cluster Survey II: Disk-Dominated Cluster Galaxies with Suppressed Star Formation
• The survival of stellar discs in Fornax-like environments, from TNG50 to real galaxies

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