Redshift evolution of the Fundamental Plane relation in the IllustrisTNG simulation

2019/06/30 by Shengdong Lu, Dandan Xu, D. Xu +9 · 24 citations
Mathematics · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics #Baryon #Dark matter #Disc galaxy #Fundamental plane (elliptical galaxies) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Gamma-ray bursts and supernovae #Geometry #Mathematics #Physics #Plane (geometry) #Redshift #Star formation #Stellar mass #Velocity dispersion #astro-ph.GA

paper · pdf · doi:10.1093/mnras/staa173

published in Monthly Notices of the Royal Astronomical Society 492(4), 5930-5939 (Oxford University Press) · 10 pages, 7 figures, 1 table. Accepted for publication in MNRAS

openalex publication_date 2020/01/27 · arxiv created 2020/01/31 · arxiv updated 2020/02/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06

Abstract

ABSTRACT We investigate the Fundamental Plane (FP) evolution of early-type galaxies in the IllustrisTNG-100 simulation (TNG100) from redshift z = 0 to z = 2. We find that a tight plane relation already exists as early as z = 2. Its scatter stays as low as ∼0.08 dex across this redshift range. Both slope parameters b and c (where R ∝ σbIc with R, σ, and I being the typical size, velocity dispersion, and surface brightness) of the plane evolve mildly since z = 2, roughly consistent with observations. The FP residual \rm Res (≡ a + blog σ + clog I - log R, where a is the zero-point of the FP) is found to strongly correlate with stellar age, indicating that stellar age can be used as a crucial fourth parameter of the FP. However, we find that 4c + b + 2 = δ, where δ ∼ 0.8 for FPs in TNG, rather than zero as is typically inferred from observations. This implies that a tight power-law relation between the dynamical mass-to-light ratio Mdyn/L and the dynamical mass Mdyn (where Mdyn ≡ 5σ2R/G, with G being the gravitational constant) is not present in the TNG100 simulation. Recovering such a relation requires proper mixing between dark matter and baryons, as well as star formation occurring with correct efficiencies at the right mass scales. This represents a powerful constraint on the numerical models, which has to be satisfied in future hydrodynamical simulations.

Citations

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