Simulating galaxy formation with the IllustrisTNG model

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

doi:10.1093/mnras/stx2656

Cited by 1,699 publications

(1,864 citation statements)

References 154 publications

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“…Future work will include validating our results with both higher-resolution simulations and improved galaxy formation models (Pillepich et al 2017;Weinberger et al 2017). Highresolution simulations of individual galaxies, at the relevant mass scales, will allow for a more realistic study of radial gradients in the IMF and fully capture the impact of star formation occurring in nuclear starbursts.…”

Section: Prospects For Future Workmentioning

confidence: 87%

“…For higher velocity dispersions, Illustris-3 exhibits shallower radial profiles at R p key galaxy properties and scaling relations, there is certainly room for improvement (Genel et al 2014;Vogelsberger et al 2014aVogelsberger et al , 2014b. For example, Illustris produced massive galaxies with too high of a stellar mass (Vogelsberger et al 2014a) and galaxy sizes that are too large (Pillepich et al 2017). In particular, relevant to studying IMF variations through the hierarchical buildup of galaxies is the merger rate.…”

Section: Simulation Limitationsmentioning

confidence: 99%

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Implications of Galaxy Buildup for Putative IMF Variations in Massive Galaxies

Blancato

Genel

Bryan

2017

ApJ

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Recent observational evidence for initial mass function (IMF) variations in massive quiescent galaxies at z=0 challenges the long-established paradigm of a universal IMF. While a few theoretical models relate the IMF to birth cloud conditions, the physical driver underlying these putative IMF variations is still largely unclear. Here we use post-processing analysis of the Illustris cosmological hydrodynamical simulation to investigate possible physical origins of IMF variability with galactic properties. We do so by tagging stellar particles in the simulation (each representing a stellar population of »  M 10 6) with individual IMFs that depend on various physical conditions, such as velocity dispersion, metallicity, or star formation rate, at the time and place in which the stars are formed. We then follow the assembly of these populations throughout cosmic time and reconstruct the overall IMF of each z=0 galaxy from the many distinct IMFs it is composed of. Our main result is that applying the observed relations between IMF and galactic properties to the conditions at the star formation sites does not result in strong enough IMF variations between z=0 galaxies. Steeper physical IMF relations are required for reproducing the observed IMF trends, and some stellar populations must form with more extreme IMFs than those observed. The origin of this result is the hierarchical nature of massive galaxy assembly, and it has implications for the reliability of the strong observed trends, for the ability of cosmological simulations to capture certain physical conditions in galaxies, and for theories of star formation aiming to explain the physical origin of a variable IMF.

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Section: Prospects For Future Workmentioning

confidence: 87%

Section: Simulation Limitationsmentioning

confidence: 99%

Implications of Galaxy Buildup for Putative IMF Variations in Massive Galaxies

Blancato

Genel

Bryan

2017

ApJ

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“…It uses 1504 3 SPH and dark matter (DM) particles. The TNG-100 simulation (Pillepich et al 2018) uses the AREPO (Springel 2010) moving mesh hydro solver in a volume of 110 3 Mpc 3 with 1820 3 DM particles and initial gas cells. Both simulations have ∼ 1 kpc gravitational softening lengths and gas and stellar mass resolutions of ∼ 10 6 M .…”

Section: Simulationsmentioning

confidence: 99%

“…Extended hot X-ray coronae have long been theorized to supply the gas necessary for star-formation in disc galaxies (Spitzer 1956;White & Rees 1978). White & Frenk (1991) predicted emission levels that should have Forman et al 1985;O'Sullivan et al 2001;Goulding et al 2016), whilst stacking ROSAT all-sky survey data about the coordinates of mainly early-type galaxies has revealed a strong correlation between the inferred CGM mass fraction and galaxy mass (Anderson et al 2015). Detections associated with individual disc galaxies are primarily limited to rare, massive cases (e.g.…”

Section: Introductionmentioning

confidence: 99%

EAGLE and Illustris-TNG Predictions for Resolved eROSITA X-Ray Observations of the Circumgalactic Medium around Normal Galaxies

Oppenheimer

Bogdán

Crain

et al. 2020

ApJL

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We simulate stacked observations of nearby hot X-ray coronae associated with galaxies in the EAGLE and Illustris-TNG hydrodynamic simulations. A forward modeling pipeline is developed to predict 4year eROSITA observations and stacked image analysis, including the effects of instrumental and astrophysical backgrounds. We propose an experiment to stack z ≈ 0.01 galaxies separated by specific star-formation rate (sSFR) to examine how the hot (T ≥ 10 6 K) circumgalactic medium (CGM) differs for high-and low-sSFR galaxies. The simulations indicate that the hot CGM of low-mass (M * ≈ 10 10.5 M ), high-sSFR (defined as the top one-third ranked by sSFR) central galaxies will be detectable to a galactocentric radius r ≈ 30 − 50 kpc. Both simulations predict lower luminosities at fixed stellar mass for the low-sSFR galaxies (the lower third of sSFR) with Illustris-TNG predicting 3× brighter coronae around high-sSFR galaxies than EAGLE. Both simulations predict detectable emission out to r ≈ 150 − 200 kpc for stacks centered on high-mass (M * ≈ 10 11.0 M ) galaxies, with EAGLE predicting brighter X-ray halos. The extended soft X-ray luminosity correlates strongly and positively with the mass of circumgalactic gas within the virial radius (f CGM ). Prior analyses of both simulations have established that f CGM is reduced by expulsive feedback driven mainly by black hole growth, which quenches galaxy growth by inhibiting replenishment of the ISM. Both simulations predict that eROSITA stacks should not only conclusively detect and resolve the hot CGM around L * galaxies for the first time, but provide a powerful probe of how the baryon cycle operates, for which there remains an absence of consensus between state-of-the-art simulations.

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“…These aspects of galaxy evolution will automatically be addressed by cosmological hydrodynamical simulations as their resolution and the realism of their subgrid modelling are improved (see e.g. Schaye et al 2015;Davé et al 2016;Dubois et al 2016;Pillepich et al 2018, for recent advances) but the computational expense of such simulations makes it difficult to treat large volumes at high resolution or to survey the parameter space of their subgrid models. The dramatic speed-up afforded by semi-analytic simulations solves these last two problems at the expense of a much more schematic representation of hydrodynamic processes and galaxy structure.…”

Section: Introductionmentioning

confidence: 99%

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Henriques

Yates

et al. 2019

Monthly Notices of the Royal Astronomical Society

112

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We have updated the Munich galaxy formation model, L-galaxies, to follow the radial distributions of stars and atomic and molecular gas in galaxy discs. We include an H 2 -based star-formation law, as well as a detailed chemical-enrichment model with explicit mass-dependent delay times for SN-II, SN-Ia and AGB stars. Information about the star formation, feedback and chemical-enrichment histories of discs is stored in 12 concentric rings. The new model retains the success of its predecessor in reproducing the observed evolution of the galaxy population, in particular, stellar mass functions and passive fractions over the redshift range 0 z 3 and mass range 8 log(M * / M ) 12, the black hole-bulge mass relation at z = 0, galaxy morphology as a function of stellar mass and the mass-metallicity relations of both stellar and gas components. In addition, its detailed modelling of the radial structure of discs allows qualitatively new comparisons with observation, most notably with the relative sizes and masses of the stellar, atomic and molecular components in discs. Good agreement is found with recent data. Comparison of results obtained for simulations differing in mass resolution by more than two orders of magnitude shows that all important distributions are numerically well converged even for this more detailed model. An examination of metallicity and surface-density gradients in the stars and gas indicates that our new model, with star formation, chemical enrichment and feedback calculated self-consistently on local disc scales, reproduces some but not all of the trends seen in recent many-galaxy IFU surveys.

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Simulating galaxy formation with the IllustrisTNG model

Cited by 1,699 publications

References 154 publications

Implications of Galaxy Buildup for Putative IMF Variations in Massive Galaxies

Implications of Galaxy Buildup for Putative IMF Variations in Massive Galaxies

EAGLE and Illustris-TNG Predictions for Resolved eROSITA X-Ray Observations of the Circumgalactic Medium around Normal Galaxies

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

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