First results from the IllustrisTNG simulations: matter and galaxy clustering

Springel, Volker; Pakmor, Rüdiger; Pillepich, Annalisa; Weinberger, Rainer; Nelson, Dylan; Hernquist, Lars; Vogelsberger, Mark; Genel, Shy; Torrey, Paul; Marinacci, Federico; Naiman, Jill

doi:10.1093/mnras/stx3304

Cited by 1,547 publications

(1,392 citation statements)

References 117 publications

(192 reference statements)

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“…Weinberger et al (2018) and Pillepich et al (2018a) provide a complete description of the physical models. Additional details about these simulations are given by Pillepich et al (2018b), Springel et al (2018), Nelson et al (2018), Naiman et al (2018), and Marinacci et al (2018).…”

Section: The Illustristng Simulationsmentioning

confidence: 99%

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Patton

Wilson

Metrow

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use the IllustrisTNG cosmological hydrodynamical simulations to investigate how the specific star formation rates (sSFRs) of massive galaxies (M * > 10 10 M ) depend on the distance to their closest companions. We estimate sSFR enhancements by comparing with control samples that are matched in redshift, stellar mass, local density and isolation, and we restrict our analysis to pairs with stellar mass ratios of 0.1 to 10. At small separations (∼ 15 kpc), the mean sSFR is enhanced by a factor of 2.0 ± 0.1 in the flagship (110.7 Mpc) 3 simulation (TNG100-1). Statistically significant enhancements extend out to 3D separations of 280 kpc in the (302.6 Mpc) 3 simulation (TNG300-1). We find similar trends in the EAGLE and Illustris simulations, although their sSFR enhancements are lower than those in TNG100-1 by about a factor of two. Enhancements in IllustrisTNG galaxies are seen throughout the redshift range explored (0 z < 1), with the strength of the enhancements decreasing with increasing redshift for galaxies with close companions. In order to more closely compare with observational results, we separately consider 2D projected distances between galaxies in IllustrisTNG. We detect significant sSFR enhancements out to projected separations of 260 kpc in TNG300-1, with projection effects diluting the size of the enhancements by about 20 per cent below 50 kpc. We find similar sSFR enhancements in TNG100-1 and Sloan Digital Sky Survey galaxies, with enhancements extending out to projected separations of about 150 kpc for star-forming galaxies at z < 0.2. Finally, by summing over all separations, we estimate that the presence of closest companions boosts the average sSFR of massive galaxies in TNG100-1 by 14.5 per cent.

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Section: The Illustristng Simulationsmentioning

confidence: 99%

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Patton

Wilson

Metrow

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…IllustrisTNG (Pillepich et al 2018b;Nelson et al 2018b;Springel et al 2018;Marinacci et al 2018;Naiman et al 2018;Nelson et al 2019) is a follow-up to the Illustris simulations (Vogelsberger et al 2014) based on the deformable-mesh hydroydynamics solver, Arepo (Springel 2010). As detailed in Pillepich et al (2018b), the stellar mass functions and stellar mass to halo mass relations are in reasonable agreement with observational and empirical constraints.…”

Section: Simulations and Halo Populationsmentioning

confidence: 99%

Stellar property statistics of massive haloes from cosmological hydrodynamics simulations: common kernel shapes

Anbajagane

Evrard

Farahi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study stellar property statistics, including satellite galaxy occupation, of massive halo populations realized by three cosmological hydrodynamics simulations: BA-HAMAS + MACSIS, TNG300 of the IllustrisTNG suite, and Magneticum Pathfinder. The simulations incorporate independent sub-grid methods for astrophysical processes with spatial resolutions ranging from 1.5 to 6 kpc, and each generates samples of 1000 or more halos with M halo > 10 13.5 M at redshift z = 0. Applying localized, linear regression (LLR), we extract halo mass-conditioned statistics (normalizations, slopes, and intrinsic covariance) for a three-element stellar property vector consisting of: i) N sat , the number of satellite galaxies with stellar mass, M > 10 10 M within radius R 200c of the halo; ii) M ,tot , the total stellar mass within that radius, and; iii) M ,BCG , the gravitationally-bound stellar mass of the central galaxy within a 100 kpc radius. Scaling parameters for the three properties with halo mass show mild differences among the simulations, in part due to numerical resolution, but there is qualitative agreement on property correlations, with halos having smaller than average central galaxies tending to also have smaller total stellar mass and a larger number of satellite galaxies. Marginalizing over total halo mass, we find the satellite galaxy kernel, p(ln N sat | M halo , z) to be consistently skewed left, with skewness parameter γ = −0.91 ± 0.02, while that of ln M ,tot is closer to log-normal, in all three simulations. The highest resolution simulations find γ −0.8 for the z = 0 shape of p(ln M ,BCG | M halo , z) and also that the fractional scatter in total stellar mass is below 10 percent in halos more massive than 10 14.3 M . We provide a Gaussian mixture fit to the low redshift N sat kernel as well as LLR parameters tabulated for halos more massive than 10 13.5 M in all simulations.

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“…The sample and measured quantities are derived from the TNG300 solution of the IllustrisTNG project 1 . Our sample consists of a subset of data that is provided publicly by the IllustrisTNG team (Nelson et al 2018;Pillepich et al 2018a;Springel et al 2018;Marinacci et al 2018;Naiman et al 2018).…”

Section: The Samplementioning

confidence: 99%

Aging haloes: implications of the magnitude gap on conditional statistics of stellar and gas properties of massive haloes

Farahi

Trac

2020

Monthly Notices of the Royal Astronomical Society

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Cold dark matter model predicts that the large-scale structure grows hierarchically. Small dark matter halos form first. Then, they grow gradually via continuous merger and accretion. These halos host the majority of baryonic matter in the Universe in the form of hot gas and cold stellar phase. Determining how baryons are partitioned into these phases requires detailed modeling of galaxy formation and their assembly history. It is speculated that formation time of the same mass halos might be correlated with their baryonic content. To evaluate this hypothesis, we employ halos of mass above 10 14 M realized by TNG300 solution of the IllustrisTNG project. Formation time is not directly observable. Hence, we rely on the magnitude gap between the brightest and the fourth brightest halo galaxy member, which is shown that traces formation time of the host halo. We compute the conditional statistics of the stellar and gas content of halos conditioned on their total mass and magnitude gap. We find a strong correlation between magnitude gap and gas mass, BCG stellar mass, and satellite galaxies stellar mass, but not the total stellar mass of halo. Conditioning on the magnitude gap can reduce the scatter about halo property-halo mass relation and has a significant impact on the conditional covariance. Reduction in the scatter can be as significant as 30%, which implies more accurate halo mass prediction. Incorporating the magnitude gap has a potential to improve cosmological constraints using halo abundance and allows us to gain insight into the baryon evolution within these systems.

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First results from the IllustrisTNG simulations: matter and galaxy clustering

Cited by 1,547 publications

References 117 publications

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Stellar property statistics of massive haloes from cosmological hydrodynamics simulations: common kernel shapes

Aging haloes: implications of the magnitude gap on conditional statistics of stellar and gas properties of massive haloes

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