TY - JOUR
T1 - The Three Hundred project
T2 - The stellar and gas profiles
AU - Li, Qingyang
AU - Cui, Weiguang
AU - Yang, Xiaohu
AU - Rasia, Elena
AU - Dave, Romeel
AU - De Petris, Marco
AU - Knebe, Alexander
AU - Peacock, John A.
AU - Pearce, Frazer
AU - Yepes, Gustavo
N1 - Funding Information:
The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gauss-centre.eu) and the Partnership for Advanced Supercomputing in Europe (PRACE, www.prace-ri.eu) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, www.lrz.de).
Funding Information:
WC and JAP acknowledge supported from the European Research Council under grant number 670193. AK and GY are supported by the Ministerio de Economía y Competitividad and the Fondo Europeo de Desarrollo Regional (MINECO/FEDER, UE) in Spain through grant AYA2015-63810-P and MICIU/FEDER through grant PGC2018-094975-C21. AK further acknowledges funding through the Spanish Red Consolider MultiDark FPA2017-90566-REDC and thanks Blumfeld for l’etat et moi. XY is supported by the National Science Foundation of China (NSFC, grant nos. 11890692, 11833005, 11621303) and the 111 Project no. B20019.
Publisher Copyright:
© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2020/5/14
Y1 - 2020/5/14
N2 - Using the catalogues of galaxy clusters from The Three Hundred project, modelled with both hydrodynamic simulations (gadget-x and gadget-music), and semi-Analytical models (SAMs), we study the scatter and self-similarity of the profiles and distributions of the baryonic components of the clusters: The stellar and gas mass, metallicity, the stellar age, gas temperature, and the (specific) star formation rate. Through comparisons with observational results, we find that the shape and the scatter of the gas density profiles matches well the observed trends including the reduced scatter at large radii which is a signature of self-similarity suggested in previous studies. One of our simulated sets, gadget-x, reproduces well the shape of the observed temperature profile, while gadget-music has a higher and flatter profile in the cluster centre and a lower and steeper profile at large radii. The gas metallicity profiles from both simulation sets, despite following the observed trend, have a relatively lower normalization. The cumulative stellar density profiles from SAMs are in better agreement with the observed result than both hydrodynamic simulations which show relatively higher profiles. The scatter in these physical profiles, especially in the cluster centre region, shows a dependence on the cluster dynamical state and on the cool-core/non-cool-core dichotomy. The stellar age, metallicity, and (s)SFR show very large scatter, which are then presented in 2D maps. We also do not find any clear radial dependence of these properties. However, the brightest central galaxies have distinguishable features compared to the properties of the satellite galaxies.
AB - Using the catalogues of galaxy clusters from The Three Hundred project, modelled with both hydrodynamic simulations (gadget-x and gadget-music), and semi-Analytical models (SAMs), we study the scatter and self-similarity of the profiles and distributions of the baryonic components of the clusters: The stellar and gas mass, metallicity, the stellar age, gas temperature, and the (specific) star formation rate. Through comparisons with observational results, we find that the shape and the scatter of the gas density profiles matches well the observed trends including the reduced scatter at large radii which is a signature of self-similarity suggested in previous studies. One of our simulated sets, gadget-x, reproduces well the shape of the observed temperature profile, while gadget-music has a higher and flatter profile in the cluster centre and a lower and steeper profile at large radii. The gas metallicity profiles from both simulation sets, despite following the observed trend, have a relatively lower normalization. The cumulative stellar density profiles from SAMs are in better agreement with the observed result than both hydrodynamic simulations which show relatively higher profiles. The scatter in these physical profiles, especially in the cluster centre region, shows a dependence on the cluster dynamical state and on the cool-core/non-cool-core dichotomy. The stellar age, metallicity, and (s)SFR show very large scatter, which are then presented in 2D maps. We also do not find any clear radial dependence of these properties. However, the brightest central galaxies have distinguishable features compared to the properties of the satellite galaxies.
KW - galaxies: clusters: general
KW - galaxies: clusters: intracluster medium
KW - galaxies: general
KW - galaxies: haloes
UR - http://www.scopus.com/inward/record.url?scp=85091964361&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85091964361&partnerID=8YFLogxK
U2 - 10.1093/mnras/staa1385
DO - 10.1093/mnras/staa1385
M3 - Article
AN - SCOPUS:85091964361
VL - 495
SP - 2930
EP - 2948
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 3
ER -