The origin of scatter in the stellar mass - halo mass relation of central galaxies in the EAGLE simulation

Abstract

We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass - halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At $z=0.1$ it declines from 0.25 dex at $M_{200,\mathrm{DMO}}\approx 10^{11}$ M${}_{\odot }$ to 0.12 dex at $M_{200,\mathrm{DMO}}\approx 10^{13}$ M${}_{\odot }$, but the trend is weak above $10^{12}$ M${}_{\odot }$. For $M_{200,\mathrm{DMO}}<10^{12.5}$ M${}_{\odot }$ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, $V_{\max ,\mathrm{DMO}}$, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the $M_{\mathrm{star}}-M_{200,\mathrm{DMO}}$ relation, and it does not explain the scatter in $M_{\mathrm{star}}-V_{\max ,\mathrm{DMO}}$. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects.

Main text 15 pages. MNRAS accepted. Added references

References in corpus (16)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
• The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
• Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations
• The spin and shape of dark matter haloes in the Millennium simulation of a LambdaCDM universe
• Baryon effects on the internal structure of LCDM halos in the EAGLE simulations
• The dark nemesis of galaxy formation: why hot haloes trigger black hole growth and bring star formation to an end
• On the Lack of Evolution in Galaxy Star Formation Efficiency
• The pseudo-evolution of halo mass
• The stellar-to-halo mass relations of local galaxies segregates by color
• Void Statistics in Large Galaxy Redshift Surveys: Does Halo Occupation of Field Galaxies Depend on Environment?
• The effect of baryons on the inner density profiles of rich clusters
• Simulation techniques for cosmological simulations
• The nature of assembly bias - I. Clues from a LCDM cosmology
• Testing cold dark matter with the low mass Tully-Fisher relation
• Testing Galaxy Quenching Theories with Scatter in the Stellar to Halo Mass Relation

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