Formation of massive disk galaxies in the IllustrisTNG simulation

Abstract

We investigate the formation history of massive disk galaxies in hydro-dynamical simulation--the IllustrisTNG, to study why massive disk galaxies survive through cosmic time. 83 galaxies in the simulation are selected with M${}_{\ast ,z=0}$ $>8\times 10^{10}$ M${}_{\odot }$ and kinematic bulge-to-total ratio less than $0.3$. We find that 8.4 percent of these massive disk galaxies have quiet merger histories and preserve disk morphology since formed. 54.2 percent have a significant increase in bulge components in history, then become disks again till present time. The rest 37.3 percent experience prominent mergers but survive to remain disky. While mergers and even major mergers do not always turn disk galaxies into ellipticals, we study the relations between various properties of mergers and the morphology of merger remnants. We find a strong dependence of remnant morphology on the orbit type of major mergers. Specifically, major mergers with a spiral-in falling orbit mostly lead to disk-dominant remnants, and major mergers of head-on galaxy-galaxy collision mostly form ellipticals. This dependence of remnant morphology on orbit type is much stronger than the dependence on cold gas fraction or orbital configuration of merger system as previously studied.

12 pages, 1 table, 8 figures. Accepted for publication in MNRAS

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Cited by in corpus (19)

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• MaNGA DynPop -- III. Stellar dynamics versus stellar population relations in 6000 early-type and spiral galaxies: Fundamental Plane, mass-to-light ratios, total density slopes, and dark matter fractions
• SDSS-IV MaNGA : spatial resolved properties of kinematically misaligned galaxies
• The interconnection between galaxy mergers, AGN activity and rapid quenching of star formation in simulated post-merger galaxies
• An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud AGNs
• Stellar angular momentum can be controlled from cosmological initial conditions
• Quenching of Massive Disk Galaxies in the IllustrisTNG Simulation
• SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk
• Formation of super-thin galaxies in Illustris-TNG
• The Ly$\alpha$, CIV, and HeII nebulae around J1000+0234: a galaxy pair at the center of a galaxy overdensity at $z=4.5$
• Quenched, bulge-dominated, but dynamically cold galaxies in IllustrisTNG and their real-world counterparts
• Universal bimodality in kinematic morphology and the divergent pathways to galaxy quenching
• The effects of the orbital configurations of mergers on reshaping galaxy structures
• Bar instability and formation timescale across Toomre's $Q$ parameter and central mass concentration: slow bar formation or true stability
• Reorientation Rates of Structural and Kinematic Axes in Simulated Massive Galaxies and the Origins of Prolate Rotation
• The weak connection between the stellar haloes and merger histories of Milky Way-mass galaxies
• The Nature of LoBAL QSOs: II. HST/WFC3 Observations Reveal Host Galaxies Dominated by Mergers
• The Formation of Dwarf Galaxy Disks
• Galaxy mergers can initiate quenching by unlocking an AGN-driven transformation of the baryon cycle