Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation
© 2020 The Author(s). 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 σ0.08 dex across this redshift...
| Main Authors: | , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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Oxford University Press (OUP)
2021
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| Online Access: | https://hdl.handle.net/1721.1/132569 |
| _version_ | 1826213585179639808 |
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| author | Lu, Shengdong Xu, Dandan Wang, Yunchong Mao, Shude Ge, Junqiang Springel, Volker Wang, Yuan Vogelsberger, Mark Naiman, Jill Hernquist, Lars |
| author_facet | Lu, Shengdong Xu, Dandan Wang, Yunchong Mao, Shude Ge, Junqiang Springel, Volker Wang, Yuan Vogelsberger, Mark Naiman, Jill Hernquist, Lars |
| author_sort | Lu, Shengdong |
| collection | MIT |
| description | © 2020 The Author(s). 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 σ0.08 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 Res (≡ a + b log σ + c log I - logR, 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 σ 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. |
| first_indexed | 2024-09-23T15:51:35Z |
| format | Article |
| id | mit-1721.1/132569 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T15:51:35Z |
| publishDate | 2021 |
| publisher | Oxford University Press (OUP) |
| record_format | dspace |
| spelling | mit-1721.1/1325692021-09-21T03:09:06Z Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation Lu, Shengdong Xu, Dandan Wang, Yunchong Mao, Shude Ge, Junqiang Springel, Volker Wang, Yuan Vogelsberger, Mark Naiman, Jill Hernquist, Lars © 2020 The Author(s). 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 σ0.08 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 Res (≡ a + b log σ + c log I - logR, 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 σ 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. 2021-09-20T18:23:06Z 2021-09-20T18:23:06Z 2020-11-17T15:43:12Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/132569 en 10.1093/MNRAS/STAA173 Monthly Notices of the Royal Astronomical Society Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf Oxford University Press (OUP) arXiv |
| spellingShingle | Lu, Shengdong Xu, Dandan Wang, Yunchong Mao, Shude Ge, Junqiang Springel, Volker Wang, Yuan Vogelsberger, Mark Naiman, Jill Hernquist, Lars Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation |
| title | Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation |
| title_full | Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation |
| title_fullStr | Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation |
| title_full_unstemmed | Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation |
| title_short | Redshift Evolution of the Fundamental Plane Relation in the IllustrisTNG Simulation |
| title_sort | redshift evolution of the fundamental plane relation in the illustristng simulation |
| url | https://hdl.handle.net/1721.1/132569 |
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