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Article Dans Une Revue Monthly Notices of the Royal Astronomical Society Année : 2019

The SAMI Galaxy Survey: comparing 3D spectroscopic observations with galaxies from cosmological hydrodynamical simulations

Jesse van de Sande
  • Fonction : Auteur
Claudia D.P. Lagos
  • Fonction : Auteur
Charlotte Welker
  • Fonction : Auteur
Joss Bland-Hawthorn
  • Fonction : Auteur
Felix Schulze
  • Fonction : Auteur
Rhea-Silvia Remus
  • Fonction : Auteur
Yannick Bahé
Sarah Brough
  • Fonction : Auteur
Julia J. Bryant
  • Fonction : Auteur
Luca Cortese
  • Fonction : Auteur
Scott M. Croom
  • Fonction : Auteur
Julien Devriendt
Yohan Dubois
Michael Goodwin
  • Fonction : Auteur
Iraklis S. Konstantopoulos
  • Fonction : Auteur
Jon S. Lawrence
  • Fonction : Auteur
Anne M. Medling
  • Fonction : Auteur
Christophe Pichon
Samuel N. Richards
  • Fonction : Auteur
Sebastian F. Sanchez
  • Fonction : Auteur
Nicholas Scott
  • Fonction : Auteur
Sarah M. Sweet
  • Fonction : Auteur

Résumé

Cosmological hydrodynamical simulations are rich tools to understand the build-up of stellar mass and angular momentum in galaxies, but require some level of calibration to observations. We compare predictions at |$z$| ∼ 0 from the eagle, hydrangea, horizon-agn, and magneticum simulations with integral field spectroscopic (IFS) data from the SAMI (Sydney-AAO Multi-object Integral field spectrograph) Galaxy Survey, ATLAS^3D, CALIFA (Calar Alto Legacy Integral Field Area), and MASSIVE surveys. The main goal of this work is to simultaneously compare structural, dynamical, and stellar population measurements in order to identify key areas of success and tension. We have taken great care to ensure that our simulated measurement methods match the observational methods as closely as possible, and we construct samples that match the observed stellar mass distribution for the combined IFS sample. We find that the eagle and hydrangea simulations reproduce many galaxy relations but with some offsets at high stellar masses. There are moderate mismatches in R_e (+), ε (−), σ_e (−), and mean stellar age (+), where a plus sign indicates that quantities are too high on average, and minus sign too low. The horizon-agn simulations qualitatively reproduce several galaxy relations, but there are a number of properties where we find a quantitative offset to observations. Massive galaxies are better matched to observations than galaxies at low and intermediate masses. Overall, we find mismatches in R_e (+), ε (−), σ_e (−), and (V/σ)_e (−). magneticum matches observations well: this is the only simulation where we find ellipticities typical for disc galaxies, but there are moderate differences in σ_e (−), (V/σ)_e (−), and mean stellar age (+). Our comparison between simulations and observational data has highlighted several areas for improvement, such as the need for improved modelling resulting in a better vertical disc structure, yet our results demonstrate the vast improvement of cosmological simulations in recent years.
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Dates et versions

hal-01921653 , version 1 (17-06-2023)

Identifiants

Citer

Jesse van de Sande, Claudia D.P. Lagos, Charlotte Welker, Joss Bland-Hawthorn, Felix Schulze, et al.. The SAMI Galaxy Survey: comparing 3D spectroscopic observations with galaxies from cosmological hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society, 2019, 484 (1), pp.869-891. ⟨10.1093/mnras/sty3506⟩. ⟨hal-01921653⟩
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