The Three HundredA large galaxy cluster catalogue for cosmological and astrophysical applications.
Weiguang Cui,* 1
In collaboration with the core team (Alexander Knebe, Gustavo Yepes and etc.) of thenIFTy and the Three hundred projects and the participants of the CCC workshop.
∗Departamento de Fısica Teorica,Universidad Autonoma de Madrid, 28049 Madrid, Spain
Simulated skies for new-generation spectroscopic surveys workshop at ESA, Madrid, April24, 2018
1https://weiguangcui.github.ioEmail: [email protected] 1 / 16
Background: Cluster of Galaxies:
Galaxy cluster is the final state of the hierarchical structure formation.
Typically a few Mpc across, contain ∼ 100 - 1000 luminous galaxies and many moredwarfs, masses & 1014.5M.Dark matter: ∼ 85%, gas: ∼ 13%, star: ∼ 1− 2%.It provides plentiful information for baryonic processes, galaxy formation and cosmologymodels.
Figure: The Coma cluster.
Email: [email protected] 2 / 16
Background: Cluster of Galaxies:
Galaxy cluster is the final state of the hierarchical structure formation.Typically a few Mpc across, contain ∼ 100 - 1000 luminous galaxies and many moredwarfs, masses & 1014.5M.
Dark matter: ∼ 85%, gas: ∼ 13%, star: ∼ 1− 2%.It provides plentiful information for baryonic processes, galaxy formation and cosmologymodels.
Figure: The Coma cluster.
Email: [email protected] 2 / 16
Background: Cluster of Galaxies:
Galaxy cluster is the final state of the hierarchical structure formation.Typically a few Mpc across, contain ∼ 100 - 1000 luminous galaxies and many moredwarfs, masses & 1014.5M.Dark matter: ∼ 85%, gas: ∼ 13%, star: ∼ 1− 2%.
It provides plentiful information for baryonic processes, galaxy formation and cosmologymodels.
Figure: The Coma cluster.
Email: [email protected] 2 / 16
Background: Cluster of Galaxies:
Galaxy cluster is the final state of the hierarchical structure formation.Typically a few Mpc across, contain ∼ 100 - 1000 luminous galaxies and many moredwarfs, masses & 1014.5M.Dark matter: ∼ 85%, gas: ∼ 13%, star: ∼ 1− 2%.It provides plentiful information for baryonic processes, galaxy formation and cosmologymodels.
Figure: The Coma cluster.
Email: [email protected] 2 / 16
Background: Cluster of Galaxies:
Galaxy cluster is the final state of the hierarchical structure formation.Typically a few Mpc across, contain ∼ 100 - 1000 luminous galaxies and many moredwarfs, masses & 1014.5M.Dark matter: ∼ 85%, gas: ∼ 13%, star: ∼ 1− 2%.It provides plentiful information for baryonic processes, galaxy formation and cosmologymodels.
Figure: The Coma cluster.
Email: [email protected] 2 / 16
Background: Cluster of Galaxies:
To understand these observational results, especially how they are formed, we needsimulations.
WeiguangCui
Email: [email protected] 3 / 16
The Three Hundred: A successor of the nIFTy project
The nIFTy galaxy cluster comparison project2
11 different (in both algorithms and baryon models) simulation codes are used to simulate thesame galaxy cluster.
2Ref: Sembolini et al. 2016a,b; Elahi et al. 2016; Cui et al. 2016; Arthur et al. 2017Email: [email protected] 4 / 16
The Three Hundred: A successor of the nIFTy project
What did we find? IThe modern SPH codes produce correct entropy profiles as AMR, moving mesh.The baryon models have larger effects than the fluid simulating techniques by mixing the entropy profiles.
Email: [email protected] 4 / 16
Entropyprofile.Ref:Sembolini etal. 2016a,b.
The Three Hundred: A successor of the nIFTy project
What did we find? IIDifferent baryon models produce similar global properties, large scatter at small scales.
Email: [email protected] 4 / 16
E.g. Baryon effects on densityprofile.Ref: Cui et al. 2016
The Three Hundred: A successor of the nIFTy project
What’s next?
Aim: to understand the formation and evolution of galaxy clusters.Comparisons between models to understand the theoretical predictions.Comparisons between models and observations to constrain the models.
A large cluster sample!
Email: [email protected] 4 / 16
The Three Hundred: Basic information
The most massive (Mvir > 8× 1014 h−1 M) 324 clusters are selected from theMultiDark simulation(MDPL2)2.324 zoomed-in ICs are generated by cutting a spherical region with a radius of15 h−1 Mpc from the cluster center.
Table: Parameters of the Three Hundred simulationsParameter Value DescriptionΩM 0.307 Total Matter density parameterΩB 0.048 Baryon density parameterΩΛ 0.693 Cosmological Constant density parameterh 0.678 Hubble constant in units of 100 km/s/Mpcσ8 0.823 Normalization of Power spectrumns 0.96 Power indexzinit 120 Initial redshift of the simulationsεphys 6.5 Plummer equivalent softening in h−1 kpcParticle mass 2.36 (12.7) gas (dark matter) particle mass in [108 h−1 M]
2https://www.cosmosim.orgEmail: [email protected] 5 / 16
The Three Hundred: theoretical models
hydrodynamical simulations with baryonicmodels:Gadget-MUSIC: classic SPH method. Radiativecooling, star formation with both thermal andkinetic Supernove (SN) feedback.Gadget-X: modern SPH with the Wendland C4kernel. Gas cooling with metal contributions, starformation with chemical enrichment, SN feedbackwith AGB phase, and AGN feedback.GIZMO: running.Gadget-PESPH: running.
SAMs from MultiDark-Galaxies:See Alexander’s talk for more detailsof Galacticus, SAG (see alsosofia’s talk) and SAGE (see alsoDarren’s talk).Notes: We select these cataloguesfrom the same regions as thehydrodynamical simulations.
Email: [email protected] 6 / 16
The Three Hundred: the cataloguesHalos and subhalos in hydrodynamical simulations are identified with AHF (Ref: Knollmann &Knebe 2009).
1013 1014 1015
M200 [M /h]
100
101
102
103
N
1013 1014 1015
M500 / [M /h]
100
101
102
103 MDPL2GadgetMUSICGadgetX
Figure: Cumulative halo mass functions. Cui et al. in prep.Email: [email protected] 7 / 16
The Three Hundred: the catalogues
Halos and subhalos in hydrodynamical simulations are identified with AHF (Ref: Knollmann &Knebe 2009).
Table: The complete sample of the Three Hundred cluster catalogues at different redshifts.
redshift M200c N200c M500c N500c[1014 h−1 M] MUSIC/X [1014 h−1 M] MUSIC/X
0.0 6.41 324 / 324 4.60 270 / 2700.5 5.02 104 / 110 3.57 94 / 1031.0 3.62 38 / 27 2.57 37 / 312.3 1.10 3 / 3 0.82 3 / 34.0 0.27 3 / 2 0.21 2 / 1
Email: [email protected] 7 / 16
The resultsThe paper will be submitted very soon.
The results are preliminary.
Email: [email protected] 8 / 16
General Properties: Baryon effects on halo mass
Figure: halo mass (M500) difference respected to the DM run. Ref: Cui et al. 2014Email: [email protected] 9 / 16
General Properties: Baryon effects on halo mass
10156 × 1014 2 × 1015
M200 [M /h]0.80
0.85
0.90
0.95
1.00
1.05
1.10
1.15
1.20
Mhy
dro/M
DM
GadgetMUSIC GadgetX
10154 × 1014 6 × 1014 2 × 1015
M500 [M /h]0.80
0.85
0.90
0.95
1.00
1.05
1.10
1.15
1.20
Figure: halo mass difference respected to the DM run. Cui et al. in prep.Email: [email protected] 9 / 16
General Properties: the dynamical stateWe applied 3 criteria to classify the cluster’s dynamical state to relaxed and un-relaxed: thevirial ratio η = (2T − Es)/|W | with 0.85 < η < 1.15, center-of-mass offset∆r = |Rcm − Rc |/R200c < 0.04 and subhalo mass fraction fs =
∑Msub/M200c < 0.1.
2.50 2.25 2.00 1.75 1.50 1.25 1.00 0.75 0.50
log10( r)0.50
0.75
1.00
1.25
1.50
1.75
2.00
2.25
=(2
TE s
)/|W
| GadgetMUSICGadgetX
1.4 1.2 1.0 0.8 0.6 0.4 0.2
log10(fs)
0
20
40
N
0 50
NFigure: The relations between the three parameters. Cui et al. in prep.
Email: [email protected] 10 / 16
General Properties: the dynamical state
We applied 3 criteria to classify the cluster’s dynamical state to relaxed and un-relaxed: thevirial ratio η = (2T − Es)/|W | with 0.85 < η < 1.15, center-of-mass offset∆r = |Rcm − Rc |/R200c < 0.04 and subhalo mass fraction fs =
∑Msub/M200c < 0.1.
Table: The fractions of relaxed clusters with differentcombinations of criteria.
M200c η, ∆r & fs ∆r & fs fs1014 h−1 M MUSIC/X MUSIC/X MUSIC/X0.10− 0.50 0.44 / 0.36 0.56 / 0.48 0.70 / 0.650.50− 1.00 0.36 / 0.34 0.45 / 0.46 0.56 / 0.571.00− 6.41 0.27 / 0.29 0.30 / 0.35 0.43 / 0.486.41− 10 0.18 / 0.21 0.20 / 0.24 0.21 / 0.26> 10 0.06 / 0.08 0.07 / 0.13 0.07 / 0.14
Table: The Cool Core cluster fraction(two methods: Rosetti et al. 2011 andcentral entropy) in the complete sample:fCC = NCC
Ntotal, the CC fraction in
dynamically relaxed clustersfCC/dr = NCC,relaxed
Nrelaxedand the relaxation
fraction in CC fdr/CC = NCC,relaxedNCC
.
Simulation fCC fCC/dr fdr/CCMUSIC 0.09 0.04 0.07X 0.26 0.33 0.21
Email: [email protected] 10 / 16
General Properties: the baryon fractions
13.0 13.5 14.0 14.5 15.0log M500 [M /h]
10 1
fract
ion
Gas fraction
GadgetMUSICGadgetX
13.0 13.5 14.0 14.5 15.0log M500 [M /h]
10 2
Stellar fraction
Kravtsov et al. 2018Gonzalez et al. 2013Zhang et al. 2011
Figure: The baryon fractions. Cui et al. in prep.Email: [email protected] 11 / 16
Optical relations
The complete sample is used here.
Figure: The optical relations. Cui et al. in prep.
Email: [email protected] 12 / 16
Optical relations: the satellite stellar mass functionThe complete sample is used here.
9.0 9.5 10.0 10.5 11.0 11.5 12.0log(M * [M /h])
100
101
102
103
N/d
log(
M*)
GadgetMUSICGadgetXGalacticusSAGSAGEYang et al. 2017: [14.4 - 14.7]Yang et al. 2017: [14.7 - 15.0]
Figure: The satellite stellar mass function. Cui et al. in prep.Email: [email protected] 13 / 16
Gas scaling relations
1013 1014 1015
M500 [M /h]
100
101
T[k
eV]
GadgetMUSIC: A=0.77, B=0.62GadgetX: A=0.78, B=0.61Vikhlinin et al. 2006Vikhlinin et al. 2009Lovisari et al. 2015GadgetMUSICGadgetX
1013 1014 1015
M500 [M /h]
10 7
10 6
10 5
10 4
10 3
d2 AY 5
00[M
pc2 ]
Planck, 2014: A=-4.19, B=1.79Nagarajan et al. 2018, A=-4.16, B=1.51GadgetMUSIC: A=-4.26, B=1.62GadgetX: A=-4.18, B=1.63GadgetMUSICGadgetX
Figure: The gas relations. Cui et al. in prep.
Email: [email protected] 14 / 16
Conclusion
The baryons have a negligible impact on the halo mass for both M200and M500.∼ 20% of the complete sample is relaxed clusters, 26% (9%) of thesample is CC for GadgetX (MUSIC).The baryon fractions are in agreement with the observations atmassive halo masses for GadgetX.The optical relations are in agreement with the observations but thegalaxies from more models seem to be a little blue.The gas relations are in agreement with observations.
Email: [email protected] 15 / 16
Future works
The density profiles, Mostoghiu et al. in prep.The environment effects, Wang et al. in prep.The mock images in optical, X-ray and SZ (lower images). And more...
WeiguangCui WeiguangCui
Email: [email protected] 16 / 16