First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time

Pillepich, Annalisa; Nelson, Dylan; Springel, Volker; Pakmor, Rüdiger; Torrey, Paul; Weinberger, Rainer; Vogelsberger, Mark; Marinacci, Federico; Genel, Shy; Wel, Arjen van der; Hernquist, Lars

doi:10.1093/mnras/stz2338

Cited by 705 publications

(755 citation statements)

References 121 publications

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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%

On the angular momentum history of galactic discs

Renzini

2020

Monthly Notices of the Royal Astronomical Society: Letters

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The stellar mass, size and rotational velocity of galactic disks all grow from redshift ∼ 2 to the present by amounts that are estimated from observationally derived scaling relations. The product of these three quantities, the angular momentum of stellar disks, is then estimated to grow by a remarkably large factor, between ∼ 20 and ∼ 50, whereas other evidences suggest a more moderate increase. This requires that the specific angular momentum of the accreted gas should systematically increase with time while remaining co-rotational with the disk over most of the last ∼ 10 Gyr. Thus, the baryonic gas vorticity of the circumgalactic medium appears to emerge as a major driver in galaxy evolution, and this paper is meant to attract attention on the sheer size of the angular momentum increase and on the need to explore to which extent this can be observed in nature and/or in simulations.

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Section: Discussionmentioning

confidence: 79%

On the angular momentum history of galactic discs

Renzini

2020

Monthly Notices of the Royal Astronomical Society: Letters

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“…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%

Limitations to the ‘basic’ HOD model and beyond

Hadzhiyska

Bose

Eisenstein

et al. 2020

Monthly Notices of the Royal Astronomical Society

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103

118

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We make use of the IllustrisTNG cosmological, hydrodynamical simulations to test fundamental assumptions of the mass-based Halo Occupation Distribution (HOD) approach to modelling the galaxy-halo connection. By comparing the clustering of galaxies measured in the 300 Mpc TNG box (TNG300) with that predicted by the standard ("basic") HOD model (bHOD), we find that, on average, the bHOD model underpredicts the real-space correlation function in the TNG300 box by ∼ 15% on scales of 1 Mpc/h < r < 20 Mpc/h, which is well beyond the target precision demanded of next-generation galaxy redshift surveys. We perform several tests to establish the robustness of our findings to systematic effects, including the effect of finite box size and the choice of halo finder. In our exploration of "secondary" parameters with which to augment the bHOD, we find that the local environment of the halo, the velocity dispersion anisotropy, β, and the product of the half-mass radius and the velocity dispersion, σ 2 R halfmass , are the three most effective measures of assembly bias that help reconcile the bHOD-predicted clustering with that in TNG300. In addition, we test other halo properties such as halo spin, formation epoch and halo concentration. We also find that at fixed halo mass, galaxies in one type of environment cluster differently from galaxies in another. We demonstrate that a more complete model of the galaxy-halo connection can be constructed if both the mass and information regarding the local environment in which a halo is embedded are combined.

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“…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%

Interacting galaxies in the IllustrisTNG simulations – II: star formation in the post-merger stage

Hani

Gosain

Ellison

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy mergers are a major evolutionary transformation whose effects are borne out by a plethora of observations and numerical simulations. However, most previous simulations have used idealised, isolated, binary mergers and there has not been significant progress on studying statistical samples of galaxy mergers in large cosmological simulations. We present a sample of 27,691 post-merger (PM) galaxies (0 ≤ z ≤ 1) identified from IllustrisTNG: a cosmological, large box, magneto-hydrodynamical simulation suite. The PM sample spans a wide range of merger and galaxy properties (M , µ, f gas ). We demonstrate that star forming (SF) PMs exhibit enhanced star formation rates (SFRs) on average by a factor of ∼ 2, while the passive PMs show no statistical enhancement. We find that the SFR enhancements: (1) show no dependence on redshift, (2) anti-correlate with the PM's stellar mass, and (3) correlate with the gas fraction of the PM's progenitors. However, SF PMs show stronger enhancements which may indicate other processes being at play (e.g., gas phase, feedback efficiency). Although the SFR enhancement correlates mildly with the merger mass ratio, the more abundant minor mergers (0.1 ≤ µ < 0.3) still contribute ∼ 50% of the total SFR enhancement. By tracing the PM sample forward in time, we find that galaxy mergers can drive significant SFR enhancements which decay over ∼ 0.5 Gyr independent of the merger mass ratio, although the decay timescale is dependent on the simulation resolution. The strongest merger-driven starburst galaxies evolve to be passive/quenched on faster timescales than their controls.

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First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time

Cited by 705 publications

References 121 publications

On the angular momentum history of galactic discs

On the angular momentum history of galactic discs

Limitations to the ‘basic’ HOD model and beyond

Interacting galaxies in the IllustrisTNG simulations – II: star formation in the post-merger stage

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