Barred galaxies in the Illustris-1 and TNG100 simulations

Abstract

We carry out a comparison study on the bar structure in the Illustris-1 and TNG100 simulations. At $z=0$, 8.9\% of 1232 disc galaxies with stellar mass $>10^{10.5}{M}_{\odot }$ in Illustris-1 are barred, while the numbers are 55\% of 1269 in TNG100. The bar fraction as a function of stellar mass in TNG100 agrees well with the survey $S^{4}G$. The median redshift of bar formation are $\sim 0.4-0.5$ and $\sim 0.25$ in TNG100 and Illustris-1 respectively. Bar fraction generally increases with stellar mass and decreases with gas fraction in both simulations. Barred galaxy had higher gas fraction at high redshift tend to form bar later. When the bars were formed, the disc gas fractions were mostly lower than 0.4. The much higher bar fraction in TNG100 probably have benefit from much lower gas fraction in massive disc galaxies since $z\sim 3$, which may result from the combination of more effective stellar and AGN feedback. The latter may be the primary factor at $z<2$. Meanwhile, in both simulations, barred galaxies have higher star formation rate before bar formation, and stronger AGN feedback all the time than unbarred galaxies. The properties of dark matter halos hosting massive disc galaxies are similar between two simulations, and should have minor effect on the different bar frequency. For individual galaxies under similar halo environment cross two simulations, different baryonic physics can lead to striking discrepancy on morphology. The morphology of individual galaxies is subject to combined effects of environment and internal baryonic physics, and is often not predictable.

22 pages, 20 figures. Accepted for publication in The Astrophysical Journal

References in corpus (16)

• 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
• Simulating galaxy formation with black hole driven thermal and kinetic feedback
• A Classical Morphological Analysis of Galaxies in the Spitzer Survey of Stellar Structure in Galaxies (S4G)
• The population of barred galaxies in the local universe I. Detection and characterisation of bars
• Bars in Disk-Dominated and Bulge-Dominated Galaxies at z~0: New Insights from ~3600 SDSS Galaxies
• Galactic Angular Momentum in the Illustris Simulation: Feedback and the Hubble Sequence
• The Dependence of Bar Frequency on Galaxy Mass, Colour, and Gas Content -- and Angular Resolution -- in the Local Universe
• Bar quenching in gas-rich galaxies
• Galaxy Zoo: Quantitative Visual Morphological Classifications for 48,000 galaxies from CANDELS
• Bar-driven evolution and quenching of spiral galaxies in cosmological simulations
• Galaxy Zoo: Morphological Classifications for 120,000 Galaxies in HST Legacy Imaging
• Effects of Gas on Formation and Evolution of Stellar Bars and Nuclear Rings in Disk Galaxies
• Stellar, gas and dark matter content of barred galaxies
• Star formation activity of barred spiral galaxies
• The morphology and kinematics of the gaseous circumgalactic medium of Milky Way mass galaxies -- II. comparison of IllustrisTNG and Illustris simulation results

Cited by in corpus (27)

• Fast galaxy bars continue to challenge standard cosmology
• A Milky Way-like barred spiral galaxy at a redshift of 3
• Morphological decomposition of TNG50 galaxies: methodology and catalogue
• Simulated Bars May Be Shorter But Are Not Slower Than Observed: TNG50 vs. MaNGA
• The Gas Morphology of Nearby Star-Forming Galaxies
• The dispersion measure of Fast Radio Bursts host galaxies: estimation from cosmological simulations
• The evolution of barred galaxies in the EAGLE simulations
• Bar-like galaxies in IllustrisTNG
• Lopsided galactic bars
• Lopsided galactic disks in IllustrisTNG
• The origin of double-peak emission-line galaxies: rotating discs, bars or galaxy mergers?
• IllustrisTNG Insights: Factors Affecting the Presence of Bars in Disk Galaxies
• Galaxy formation physics behind bar formation: A view from cosmological hydrodynamical simulations
• Unraveling Joint Evolution of Bars, Star Formation, and Active Galactic Nuclei of Disk Galaxies
• The dispersion measure and scattering of Fast Radio Bursts: contributions from multi-components, and clues for the intrinsic properties
• On the Correlation Between Atomic Gas and Bars in Galaxies
• The redshift evolution of galactic bar pattern speed in TNG50
• A morphological segmentation approach to determining bar lengths
• The role of impact parameter in typical close galaxy flybys
• Bar instability and formation timescale across Toomre's $Q$ parameter and central mass concentration: slow bar formation or true stability
• Reconciling the magnetic field in central disc galaxies with the dynamical mass using the cosmological simulations
• The evolution of the barred galaxy population in the TNG50 simulation
• Tidally induced bar-like galaxies in simulated clusters
• Disc instability and bar formation: view from the IllustrisTNG simulations
• The NewHorizon Simulation -- To Bar Or Not To Bar
• The multi-component fitting to the star formation histories in the TNG simulation
• Numerical Study of Bar Suppression in Galaxy Models Due to Disc Heating