Reconciling the magnetic field in central disc galaxies with the dynamical mass using the cosmological simulations

Abstract

The Universe is pervaded by magnetic fields in different scales, although for simplicity, they are ignored in most cosmological simulations. In this paper, we use the TNG50, which is a large cosmological galaxy formation simulation that incorporates magnetic fields with an unprecedented resolution. We study the correlation of the magnetic field with various galaxy properties such as the total, stellar and gaseous mass, circular velocity, size and star formation rate. We find a linear correlation between the average magnetic field pervading the disc of galaxies in relative isolation and their circular velocities. In addition we observed that in this sample the average magnetic field in the disc is correlated with the total mass as $\overline{B}\sim M_{\mathrm{tot},{\mathrm{R}}_{\star }}^{0.2}$. We also find that the massive galaxies with active wind-driven black hole feedback, do not follow this trend, as their magnetic field is substantially affected by this feedback mode in the TNG50 simulation. We show that the correlation of the magnetic field with the star formation rate is a little weaker than the circular velocity. Moreover, we compare the magnetic field components of the above sample with a compiled observational sample of non-cluster non-interacting nearby galaxies. Similar to the observation, we find a coupling between the ordered magnetic field and the circular velocity of the flat part of the rotation curve in the simulation, although contrary to the observation, the ordered component is dominant in the simulation.

Accepted for publication in MNRAS

References in corpus (42)

• The NumPy array: a structure for efficient numerical computation
• Properties of galaxies reproduced by a hydrodynamic simulation
• Simulating galaxy formation with black hole driven thermal and kinetic feedback
• The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time
• The dark nemesis of galaxy formation: why hot haloes trigger black hole growth and bring star formation to an end
• Galactic Angular Momentum in the Illustris Simulation: Feedback and the Hubble Sequence
• Cluster Magnetic Fields from Galactic Outflows
• Evolution of magnetic fields in galaxies and future observational tests with the Square Kilometre Array
• Magnetohydrodynamic Simulations of Disk Galaxy Formation: the Magnetization of The Cold and Warm Medium
• On the amplification of magnetic fields in cosmic filaments and galaxy clusters
• Global galactic dynamo driven by cosmic-rays and exploding magnetized stars
• First results from SMAUG: Characterization of Multiphase Galactic Outflows from a Suite of Local Star-Forming Galactic Disk Simulations
• The Turbulent Dynamo in Highly Compressible Supersonic Plasmas
• The Radio Continuum-Star Formation Rate Relation in WSRT SINGS Galaxies
• Fast galaxy bars continue to challenge standard cosmology
• X-ray bubbles in the circumgalactic medium of TNG50 Milky Way- and M31-like galaxies: signposts of supermassive black hole activity
• High-resolution radio continuum survey of M33: III. Magnetic fields
• Plasma turbulence in the interstellar medium
• How primordial magnetic fields shrink galaxies
• Simulating radio synchrotron emission in star-forming galaxies: small-scale magnetic dynamo and the origin of the far infrared-radio correlation
• Magnetic Fields in the Formation of the First Stars. I. Theory vs. Simulation
• Magnetic fields and the dynamics of spiral galaxies
• A small-scale dynamo in feedback-dominated galaxies - III. Cosmological simulations
• The many lives of active galactic nuclei-II: The formation and evolution of radio jets and their impact on galaxy evolution
• Barred galaxies in the Illustris-1 and TNG100 simulations
• Simulated Bars May Be Shorter But Are Not Slower Than Observed: TNG50 vs. MaNGA
• The High Fraction of Thin Disk Galaxies Continues to Challenge ΛCDM Cosmology
• The Circumgalactic Medium of Milky Way-like Galaxies in the TNG50 Simulation -- II: Cold, Dense Gas Clouds and High-Velocity Cloud Analogs
• Evolution of primordial magnetic fields during large-scale structure formation
• Magnetic Fields on FIRE: Comparing B-fields in the multiphase ISM and CGM of Simulated L${}_{\ast }$ Galaxies to Observations
• The global structure of magnetic fields and gas in simulated Milky Way-analogue galaxies
• Cosmic evolution of radio-AGN feedback: confronting models with data
• Where do galaxies end? Comparing measurement techniques of hydrodynamic-simulation galaxies' integrated properties
• The SATIN project I: Turbulent multi-phase ISM in Milky Way simulations with SNe feedback from stellar clusters
• Simulating large-scale structure formation with magnetic fields
• Feedback by supermassive black holes in galaxy evolution: impacts of accretion and outflows on the star formation rate
• A Subgrid Turbulent Mean Field Dynamo Model for Cosmological Galaxy Formation Simulations
• Quenching of Massive Disk Galaxies in the IllustrisTNG Simulation
• Global enhancement and structure formation of the magnetic field in spiral galaxies
• Magnetic fields do not suppress global star formation in low metallicity dwarf galaxies
• Hydrodynamic simulations of the Disk of Gas Around Supermassive black holes (HDGAS) -I; Molecular Gas Dynamics
• Bar formation in submaximal discs: a challenge for ΛCDM

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