Revealing the galaxy-halo connection in IllustrisTNG

Abstract

We use the IllustrisTNG (TNG) simulations to explore the galaxy-halo connection as inferred from state-of-the-art cosmological, magnetohydrodynamical simulations. With the high mass resolution and large volume achieved by combining the 100 Mpc (TNG100) and 300 Mpc (TNG300) volumes, we establish the mean occupancy of central and satellite galaxies and their dependence on the properties of the dark matter haloes hosting them. We derive best-fitting HOD parameters from TNG100 and TNG300 for target galaxy number densities of ${\bar{n}}_g=0.032h^3$Mpc${}^{-3}$ and ${\bar{n}}_g=0.016h^3$Mpc${}^{-3}$, respectively, corresponding to a minimum galaxy stellar mass of $M_{\star }\sim 1.9\times 10^9{\mathrm{M}}_{\odot }$ and $M_{\star }\sim 3.5\times 10^9{\mathrm{M}}_{\odot }$, respectively, in hosts more massive than $10^{11}{\mathrm{M}}_{\odot }$. Consistent with previous work, we find that haloes located in dense environments, with low concentrations, later formation times, and high angular momenta are richest in their satellite population. At low mass, highly-concentrated haloes and those located in overdense regions are more likely to contain a central galaxy. The degree of environmental dependence is sensitive to the definition adopted for the physical boundary of the host halo. We examine the extent to which correlations between galaxy occupancy and halo properties are independent and demonstrate that HODs predicted by halo mass and present-day concentration capture the qualitative dependence on the remaining halo properties. At fixed halo mass, concentration is a strong predictor of the stellar mass of the central galaxy, which may play a defining role in the fate of the satellite population. The radial distribution of satellite galaxies, which exhibits a universal form across a wide range of host halo mass, is described accurately by the best-fit NFW density profile of their host haloes.

20 pages, 13 figures, 1 table, comments welcome

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Cited by in corpus (69)

• Limitations to the "basic'' HOD model and beyond
• AbacusHOD: A highly efficient extended multi-tracer HOD framework and its application to BOSS and eBOSS data
• COSMOS2020: The cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z~5
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• Evidence for galaxy assembly bias in BOSS CMASS redshift-space galaxy correlation function
• The galaxy-halo connection of emission-line galaxies in IllustrisTNG
• Extensions to models of the galaxy-halo connection
• Baryonic Imprints on DM Halos: Population Statistics from Dwarf Galaxies to Galaxy Clusters
• On the influence of halo mass accretion history on galaxy properties and assembly bias
• Elucidating Galaxy Assembly Bias in SDSS
• The little things matter: relating the abundance of ultrafaint satellites to the hosts' assembly history
• Stellar Property Statistics of Massive Halos from Cosmological Hydrodynamics Simulations: Common Kernel Shapes
• Illustrating galaxy-halo connection in the DESI era with IllustrisTNG
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• The MillenniumTNG Project: An improved two-halo model for the galaxy-halo connection of red and blue galaxies
• The emergence of dark matter-deficient ultra-diffuse galaxies driven by scatter in the stellar mass-halo mass relation and feedback from globular clusters
• Testing the Accuracy of Halo Occupation Distribution Modelling using Hydrodynamic Simulations
• Does Concentration Drive the Scatter in the Stellar-to-Halo Mass Relation of Galaxy Clusters?
• Galaxy assembly bias of central galaxies in the Illustris simulation
• FEASTS: IGM cooling triggered by tidal interactions through the diffuse HI phase around NGC 4631
• The Signatures of Self-Interacting Dark Matter and Subhalo Disruption on Cluster Substructure
• How to Optimally Constrain Galaxy Assembly Bias: Supplement Projected Correlation Functions with Count-in-cells Statistics
• On the prospect of using the maximum circular velocity of halos to encapsulate assembly bias in the galaxy-halo connection
• How galaxies populate haloes in very low-density environments? An analysis of the Halo Occupation Distribution in cosmic voids
• Responses of Halo Occupation Distributions: a new ingredient in the halo model & the impact on galaxy bias
• MaNGIA: 10,000 mock galaxies for stellar population analysis
• On the environmental influence of groups and clusters of galaxies beyond the virial radius: Galactic conformity at few Mpc scales
• Diffstar: A Fully Parametric Physical Model for Galaxy Assembly History
• The dark side of galaxy stellar populations I: The stellar-to-halo mass relation and the velocity dispersion - halo mass relation
• Evidence of Galaxy Assembly Bias in SDSS DR7 Galaxy Samples from Count Statistics
• SHAM through the lens of a hydrodynamical simulation
• Simulation view of galaxy clusters with low X-ray surface brightness
• How do galaxies populate halos in extreme density environments? An analysis of the Halo Occupation Distribution in SDSS
• Joint galaxy-galaxy lensing and clustering constraints on galaxy formation
• Modeling assembly bias with machine learning and symbolic regression
• Modelling the galaxy-halo connection with semi-recurrent neural networks
• 2D k-th nearest neighbor statistics: a highly informative probe of galaxy clustering
• How the Galaxy-Halo Connection Depends on Large-Scale Environment
• Galaxy clustering from the bottom up: A Streaming Model emulator I
• The Beyond-Halo Mass Effects of the Cosmic Web Environment on Galaxies
• High-fidelity reproduction of central galaxy joint distributions with Neural Networks
• The dark side of galaxy stellar populations II: The dependence of star formation histories on halo mass and on the scatter of the main sequence
• Connection between galaxy morphology and dark-matter halo structure I: a running threshold for thin discs and size predictors from the dark sector
• Toward Accurate Modeling of Galaxy Clustering on Small Scales: Constraining the Galaxy-Halo Connection with Optimal Statistics
• Toward Accurate Modeling of Galaxy Clustering on Small Scales: Halo Model Extensions and Lingering Tension
• The spatial distribution of satellites in galaxy clusters
• Cosmology in the non-linear regime : the small scale miracle
• Why do semi-analytic models predict higher scatter in the stellar mass-halo mass relation than cosmological hydrodynamic simulations?
• Satellite galaxy abundance dependency on cosmology in Magneticum simulations
• Unraveling emission line galaxy conformity at z~1 with DESI early data
• An Improved and Physically-Motivated Scheme for Matching Galaxies with Dark Matter Halos
• The circular velocity and halo mass functions of galaxies in the nearby Universe
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• Conditional Colour-Magnitude Distribution of Central Galaxies in Galaxy Formation Models
• How do uncertainties in galaxy formation physics impact field-level galaxy bias?
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• One Stream or Two -- Exploring Andromeda's North West Stream
• Exploring the halo-galaxy connection with probabilistic approaches
• A Conditional Abundance Matching Method of Extending Simulated Halo Merger Trees to Resolve Low-Mass Progenitors and Sub-halos
• The Outskirt Stellar Mass of Low-Redshift Massive Galaxies is an Excellent Halo Mass Proxy in Illustris/IllustrisTNG Simulations
• Predicting halo occupation and galaxy assembly bias with machine learning
• Gravitational potential drives the concentration dependence of the stellar mass-halo mass relation
• The PARADIGM project II: The lifetimes and quenching of satellites in Milky Way-mass haloes
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• Constraining Galaxy-Halo Connection Using Machine Learning
• Exploiting Non-linear Scales in Galaxy-Galaxy Lensing and Galaxy Clustering: A Forecast for the Dark Energy Survey
• Exploring the effect of baryons on the radial distribution of satellite galaxies with GAMA and IllustrisTNG
• Mimicking the halo-galaxy connection using machine learning