The Three Hundred - A large galaxy cluster catalogue for cosmological and astrophysical

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

https://weiguangcui.github.io

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


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.




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.




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.




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.




To understand these observational results, especially how they are formed, we needsimulations.

WeiguangCui


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


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.


Entropyprofile.Ref:Sembolini etal. 2016a,b.


What did we find? IIDifferent baryon models produce similar global properties, large scatter at small scales.


E.g. Baryon effects on densityprofile.Ref: Cui et al. 2016


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!


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

https://www.cosmosim.org

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.


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


The resultsThe paper will be submitted very soon.

The results are preliminary.


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.


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


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.


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.


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.


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


The Three Hundred - A large galaxy cluster catalogue for cosmological and astrophysical

Documents