2019
DOI: 10.1093/mnras/stz2338
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First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time

Abstract: We present a new cosmological, magnetohydrodynamical simulation for galaxy formation: TNG50, the third and final installment of the IllustrisTNG project. TNG50 evolves 2 × 2160 3 dark-matter particles and gas cells in a volume 50 comoving Mpc across. It hence reaches a numerical resolution typical of zoom-in simulations, with a baryonic element mass of 8.5 × 10 4 M and an average cell size of 70 − 140 parsecs in the star-forming regions of galaxies. Simultaneously, TNG50 samples ∼700 (6,500) galaxies with stel… Show more

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Cited by 700 publications
(755 citation statements)
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“…In the simulation discussed by Pillepich et al (2019) disk radii grow by a large factor since z ∼ 2, especially for M * > 10 10 M⊙, (see their Figure B1), that, coupled with the large expected increase in stellar mass, implies indeed a large increase of the AM of the stellar disks. Again, this means that, to some extent, the simulation does produce a CGM with sufficient vorticity to drive the disk growth together with its AM, in a roughly consistent fashion with what indicated by the scaling relations, as quantified in Section 1.…”
Section: Discussionmentioning
confidence: 79%
“…In the simulation discussed by Pillepich et al (2019) disk radii grow by a large factor since z ∼ 2, especially for M * > 10 10 M⊙, (see their Figure B1), that, coupled with the large expected increase in stellar mass, implies indeed a large increase of the AM of the stellar disks. Again, this means that, to some extent, the simulation does produce a CGM with sufficient vorticity to drive the disk growth together with its AM, in a roughly consistent fashion with what indicated by the scaling relations, as quantified in Section 1.…”
Section: Discussionmentioning
confidence: 79%
“…Since a high value of the beta parameter implies a weaker clustering signal (Faltenbacher & White 2010;Ramakrishnan et al 2019), for our reordering test we assign higher number of galaxies to halos with smaller dispersion anisotropy, analogously to how we treat next the velocity dispersion as a secondary parameter. The effect of this can be seen in Fig.…”
Section: Velocity Anisotropymentioning
confidence: 99%
“…However, fully investigating the merger-induced SFR budget requires a much higher mass resolution. Such a study will be possible with the forthcoming IllustrisTNG50 simulation (Nelson et al 2019b;Pillepich et al 2019).…”
Section: Q(ssf R)mentioning
confidence: 99%