The evolution of the barred galaxy population in the TNG50 simulation

Abstract

We use the magnetic-hydrodynamical simulation TNG50 to study the evolution of barred massive disc galaxies. Massive spiral galaxies are already present as early as $z=4$, and bar formation takes place already at those early times. The bars grow longer and stronger as the host galaxies evolve, with the bar sizes increasing at a pace similar to that of the disc scale lengths. The bar fraction mildly evolves with redshift for galaxies with $M_{\ast }\ge 10^{10}M\odot$, being greater than $\sim 40\%$ at $0.5<z<3$ and $\sim 30\%$ at $z=0$. When bars larger than a given physical size ($\ge 2\mathrm{kpc}$) or the angular resolution limit of twice the I-band angular PSF FWHM of the HST are considered, the bar fraction dramatically decreases with increasing redshift, reconciling the theoretical predictions with observational data. We find that barred galaxies have an older stellar population, lower gas fractions and star formation rates than unbarred galaxies. In most cases, the discs of barred galaxies assembled earlier and faster than the discs of unbarred galaxies. We also find that barred galaxies are typical in haloes with larger concentrations and smaller spin parameters than unbarred galaxies. Furthermore, the inner regions of barred galaxies are more baryon-dominated than those of unbarred galaxies but have comparable global stellar mass fractions. Our findings suggest that the bar population could be used as a potential tracer of the buildup of disc galaxies and their host haloes. With this paper, we release a catalogue of barred galaxies in TNG50 at $6$ redshifts between $z=4$ and $z=0$.

arXiv comment19 pages and 16 figures. Accepted in MNRAS and published catalogues in https://www.tng-project.org/data/docs/specifications/\#sec5j

References in corpus (100)

• Planck 2015 results. XIII. Cosmological parameters
• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• Populating a cluster of galaxies - I. Results at z=0
• E pur si muove: Galiliean-invariant cosmological hydrodynamical simulations on a moving mesh
• How Do Galaxies Get Their Gas?
• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• 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
• 3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since $z=3$
• Properties of galaxies reproduced by a hydrodynamic simulation
• 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
• First results from the IllustrisTNG simulations: radio haloes and magnetic fields
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time
• Mass assembly in quiescent and star-forming galaxies since z=4 from UltraVISTA
• First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback
• A model for cosmological simulations of galaxy formation physics
• A universal angular momentum profile for galactic halos
• First Results from the TNG50 Simulation: The evolution of stellar and gaseous disks across cosmic time
• Galaxies in a simulated $\Lambda$CDM Universe I: cold mode and hot cores
• The merger rate of galaxies in the Illustris Simulation: a comparison with observations and semi-empirical models
• The Illustris simulation: the evolving population of black holes across cosmic time
• What determines the strength and the slowdown rate of bars ?
• Simulations of Galaxy Formation in a Lambda CDM Universe II: The Fine Structure of Simulated Galactic Disks
• Compaction and Quenching of High-z Galaxies in Cosmological Simulations: Blue and Red Nuggets
• The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time
• Constraints from Dynamical Friction on the Dark Matter Content of Barred Galaxies
• Structural Properties of Pseudo-Bulges, Classical Bulges and Elliptical Galaxies: an SDSS Perspective
• Forming Realistic Late-Type Spirals in a LCDM Universe: The Eris Simulation
• The Illustris Simulation: Public Data Release
• Dynamics of Barred Galaxies
• Morphology, photometry and kinematics of N-body bars. I Three models with different halo central concentrations
• The Secular Evolution of Disk Structural Parameters
• EMERGE - An empirical model for the formation of galaxies since $z\sim 10$
• Evolution of the Bar Fraction in COSMOS: Quantifying the Assembly of the Hubble Sequence
• The formation of disc galaxies in high resolution moving-mesh cosmological simulations
• Bar formation and evolution in disc galaxies with gas and a triaxial halo: Morphology, bar strength and halo properties
• The population of barred galaxies in the local universe I. Detection and characterisation of bars
• Galaxy Zoo: Bars in Disk Galaxies
• The Size Evolution of Star-forming and Quenched Galaxies in the IllustrisTNG simulation
• The Origin of Disks and Spheroids in Simulated Galaxies
• The Central Region of Barred Galaxies: Molecular Environment, Starbursts, and Secular Evolution
• How Large Are the Bars in Barred Galaxies?
• 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
• A dynamically cold disk galaxy in the early Universe
• The Dependence of Bar Frequency on Galaxy Mass, Colour, and Gas Content -- and Angular Resolution -- in the Local Universe
• Galaxy Zoo and ALFALFA: Atomic Gas and the Regulation of Star Formation in Barred Disc Galaxies
• The two-phase formation history of spiral galaxies traced by the cosmic evolution of the bar fraction
• Can bars be destroyed by a central mass concentration? I. Simulations
• Galaxy Zoo: Observing Secular Evolution Through Bars
• The Evolution of Barred Spiral Galaxies in the Hubble Deep Fields North and South
• Chemodynamics of barred galaxies in cosmological simulations: On the Milky Way's quiescent merger history and in-situ bulge
• Galaxy Zoo: An independent look at the evolution of the bar fraction over the last eight billion years from HST-COSMOS
• High redshift JWST predictions from IllustrisTNG: Dust modelling and galaxy luminosity functions
• Secular Evolution and Structural Properties of Stellar Bars in Galaxies
• A Cold, Massive, Rotating Disk Galaxy 1.5 Billion Years after the Big Bang
• A Constant Bar Fraction out to Redshift z~1 in the Advanced Camera for Surveys Field of the Tadpole Galaxy
• Bulges or Bars from Secular Evolution?
• A massive stellar bulge in a regularly rotating galaxy 1.2 billion years after the Big Bang
• Early structure in LCDM
• Rotation Curves in z~1-2 Star-Forming Disks: Evidence for Cored Dark Matter Distributions
• Galaxy Zoo: CANDELS Barred Disks and Bar Fractions
• Barred galaxies in the EAGLE cosmological hydrodynamical simulation
• Bar-driven evolution and quenching of spiral galaxies in cosmological simulations
• Tidally induced bars in Illustris galaxies
• Spinning dark matter halos promote bar formation
• Spiral Instabilities in N-body Simulations I: Emergence from Noise
• Fast rotating and low-turbulence discs at $z\simeq 4.5$: Dynamical evidence of their evolution into local early-type galaxies
• Hot Disks And Delayed Bar Formation
• Shocks and angular momentum flips: a different path to feeding the nuclear regions of merging galaxies
• Revisiting the tension between fast bars and the $\Lambda$CDM paradigm
• The buildup of strongly barred galaxies in the TNG100 simulation
• A mass threshold for galactic gas discs by spin flips
• Bar-formation as driver of gas inflows in isolated disc galaxies
• Secular Damping of Stellar Bars in Spinning Dark Matter Halos
• External versus internal triggers of bar formation in cosmological zoom-in simulations
• What Makes the Family of Barred Disc Galaxies So Rich: Damping Stellar Bars in Spinning Haloes
• Barred Galaxies in the IllustrisTNG Simulation
• Bar instability in disk-halo systems
• Bars in hydrodynamical cosmological simulations
• Simultaneous modelling of matter power spectrum and bispectrum in the presence of baryons
• The stability of stellar disks in Milky-Way sized dark matter halos
• High redshift JWST predictions from IllustrisTNG: II. Galaxy line and continuum spectral indices and dust attenuation curves
• SDSS-IV MaNGA: The link between bars and the early cessation of star formation in spiral galaxies
• The dependence of the galaxy stellar-to-halo mass relation on galaxy morphology
• Galaxy disc scaling relations: A tight linear galaxy -- halo connection challenges abundance matching
• Stellar mass distribution of S${}^4$G disk galaxies and signatures of bar-induced secular evolution
• What Determines the Sizes of Bars in Spiral Galaxies?
• Stellar, gas and dark matter content of barred galaxies
• Black Hole Starvation and Bulge Evolution in a Milky Way-like Galaxy
• Barred galaxies in the Illustris-1 and TNG100 simulations
• Stellar populations across galaxy bars in the MUSE TIMER project
• Why are some galaxies not barred?
• Massive disc galaxies in cosmological hydrodynamical simulations are too dark matter-dominated
• Automated bar detection in local disc galaxies from the SDSS - The colors of bars
• Barred galaxies in cosmological zoom-in simulations: the importance of feedback
• Bar resilience to flybys in a cosmological framework

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