First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies

By A. Pillepich, D. Nelson, L. Hernquist, Volker Springel, Rüdiger Pakmor, P. Torrey, R. Weinberger, Shy Genel, Jill P. Naiman, F. Marinacci and 1 more. 2017

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The IllustrisTNG project is a new suite of cosmological magneto-hydrodynamical simulations of galaxy formation performed with the Arepo code and updated models for feedback physics. Here we introduce the first two simulations of the series, TNG100 and TNG300, and quantify the stellar mass content of about 4000 massive galaxy groups and clusters ($10^{13} \leq M_{\rm 200c}/M_{\rm sun} \leq 10^{15}$) at recent times ($z \leq 1$). The richest clusters have half of their total stellar mass bound to satellite galaxies, with the other half being associated with the central galaxy and the diffuse intra-cluster light. The exact ICL fraction depends sensitively on the definition of a central galaxy's mass and varies in our most massive clusters between 20 to 40% of the total stellar mass. Haloes of $5\times 10^{14}M_{\rm sun}$ and above have more diffuse stellar mass outside 100 kpc than within 100 kpc, with power-law slopes of the radial mass density distribution as shallow as the dark matter's ( $-3.5 < \alpha_{\rm 3D} < -3$). Total halo mass is a very good predictor of stellar mass, and vice versa: at $z=0$, the 3D stellar mass measured within 30 kpc scales as $\propto (M_{\rm 500c})^{0.49}$ with a $\sim 0.12$ dex scatter. This is possibly too steep in comparison to the available observational constraints, even though the abundance of TNG less massive galaxies ($< 10^{11}M_{\rm sun}$ in stars) is in good agreement with the measured galaxy stellar mass functions at recent epochs. The 3D sizes of massive galaxies fall too on a tight ($\sim$0.16 dex scatter) power-law relation with halo mass, with $r^{\rm stars}_{\rm 0.5} \propto (M_{\rm 500c})^{0.53}$. Even more fundamentally, halo mass alone is a good predictor for the whole stellar mass profiles beyond the inner few kpc, and we show how on average these can be precisely recovered given a single mass measurement of the galaxy or its halo.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/96c321593aab1530455e5548a26e9629772df1f2

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Citations in the corpus

Quantifying baryon effects on the matter power spectrum and the weak lensing shear correlation (2018, methodology): “The Illustris-TNG suite [13, 79, 80] consists of magneto-hydrodynamical simulations performed with the AREPO code [81] assuming Planck cosmological parameters.”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, methodology): “The total energy available to drive winds from a gas cell therefore depends on its instantaneous star formation rate as Ėw = ew ṀSFR which is roughly ' 1041−1042 erg/s ṀSFR/(M /yr) depending on the local gas metallicity (see Pillepich et al. 2018a).”
First results from the IllustrisTNG simulations: matter and galaxy clustering (2017, methodology): “We emphasize that all model parameters of the IllustrisTNG runs have been kept exactly the same as in our default model described in Pillepich et al. (2018), and also no adjustments of these parameters are made for different numerical mass resolutions, except for the gravitational softening lengths…”
The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics (2018, background): “…star formation activity of galaxies produced in the state-ofthe-art cosmological magneto-hydrodynamical simulations of The Next Generation Illustris project (hereafter IllustrisTNG or TNG: Naiman et al. 2018; Marinacci et al. 2018; Springel et al. 2018; Pillepich et al. 2018b; Nelson et al. 2018a).”
A-type stars in the Canada–France Imaging Survey – II. Tracing the height of the disc at large distances with Blue Stragglers (2018, background): “…of the Galaxy that formed in situ and the fraction that originally came from the Galactic disc (e.g. Eggen, Lynden-Bell & Sandage 1962; Searle & Zinn 1978; Carollo et al. 2007, 2010; Font et al. 2011; Rodriguez-Gomez et al. 2016; Deason et al. 2017; Belokurov et al. 2018; Pillepich et al. 2018).”
The optical morphologies of galaxies in the IllustrisTNG simulation: a comparison to Pan-STARRS observations (2018, methodology): “MNRAS 000, 000–000 (0000) cells above a given density threshold (nH ∼ 0.1 cm−3), which are stochastically converted into stellar particles (for details, see Springel & Hernquist 2003; Vogelsberger et al. 2013; Pillepich et al. 2018a).”
simba: Cosmological simulations with black hole growth and feedback (2019, result): “(iv) Illustris-TNG uses, at maximum, 200% of the AGN bolometric luminosity (assuming a 10% radiative efficiency), whereas for our model, the maximum is approximately a third of the bolometric luminosity.”
The IllustrisTNG simulations: public data release (2018, methodology): “For complete details on the behavior, implementation, parameter selection, and validation of these physical models, see the two TNG methods papers: Weinberger et al. (2017) and Pillepich et al. (2018b).”
Ingredients for 21 cm Intensity Mapping (2018, methodology): “The numerical methods and subgrid physics models build upon Vogelsberger et al. (2013), and are specified in full in Weinberger et al. (2017a,b) and Pillepich et al. (2017b).”
First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time (2019, methodology): “As a reminder, we do not adjust in any way our model parameters as a function of numerical resolution, but for the choices on the softening lengths (see Pillepich et al. 2018a, for a discussion).”