HYDRODYNAMICAL SIMULATIONS OF GALAXY CLUSTERS

Transcription

1 HYDRODYNAMICAL SIMULATIONS OF GALAXY CLUSTERS Susana Planelles (UV/OATS) UV collaborators: V. Quilis, M. Perucho, J.M. Martí, E. Ricciardelli OATS-INAF collaborators: S. Borgani, G. Murante, E. Rasia, V. Biffi, D. Fabjan, K. Dolag, A. Beck, L. Steinborn, N. Truong Tracing Cosmic Evolution with Clusters of Galaxies Meeting Sesto, on Fundamental 1 st -5 th July 2013 Cosmology Barcelona, 15 th -17 th June 2016

2 Introduction Galaxy clusters GALAXY CLUSTERS GCs: crucial cosmological probes (e.g. Kravtsov & Borgani 2012, Planelles+14b) GC mass: crucial astrophysical and cosmological purposes Universal cluster radial profile: Cluster core: - Large scatter - BARYON PHYSICS Mid radii : - Self-similarity - X-RAYS/SZ SCALING RELATIONS Outskirts: -Deviation from HSE - GAS CLUMPING Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

3 Cosmological Simulations DIANOGA cluster set DIANOGA CLUSTER SET General properties (Bonafede+11, Planelles+14) Upgraded version of GADGET-3 (Springel 2005, Beck+15) ΛCDM: Ω m =0.24, Ω Λ =0.76, Ω b =0.04, h=0.72, σ 8 =0.8 Parent DM-only simulation: DM particles, L box =1 h -1 Gpc Re-simulation of 29 Lagrangian regions centred in clusters with M vir h -1 M (24) and M vir (1-7) h -1 M (5) Physics included (Steinborn+15) NR: non-radiative run CSF: cooling, SF, metals, SN (v w =350 km s -1 ) AGN: cooling, SF, metals, SN (v w =350 km s -1 ), AGN (Bonafede et al. 2011) The set of simulated clusters 160 systems with M vir h -1 M 70 clusters with M vir h -1 M Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

4 Scaling Relations X-ray scaling relations at z=0 X-ray scaling relations at z=0.5 SZ scaling relations at z=0 X-RAY SCALING RELATIONS AT z=0 Y X is relatively unaffected by non-gravitational physics (e.g. Kravtsov+06, Fabjan+11) AGN feedback: significant baryon depletion in poor clusters + reduction of SF (Puchwein+10, Fabjan+11, McCarthy+11, Battaglia+13, LeBrun+14, Pike+14) Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

5 Scaling Relations X-ray scaling relations at z=0 X-ray scaling relations at z=0.5 SZ scaling relations at z=0 X-RAY SCALING RELATIONS AT z=0.5 L-M: realistic simulated baryon fraction over the mass range investigated M-T: acceptable interplay of gravitational and astrophysical thermal processes (Truong et al., in prep.) Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

6 Scaling Relations X-ray scaling relations at z=0 X-ray scaling relations at z=0.5 SZ scaling relations at z=0 SZ SCALING RELATIONS AT z=0 Good agreement with observations, especially for massive systems (e.g. Marrone+12) Within R 500, there is not a significant dependence on the physics included Intrinsic scatter: ~ 7% within R 500 and ~10% within R 2500 (e.g. Nagai+06, Sembolini+13) <R 500 <R 2500 (Planelles et al., submitted) Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

7 ICM Radial Profiles Entropy and Iron profiles Pressure profiles ENTROPY AND IRON PROFILES: CC/NCC DICHOTOMY Combined action of AGN feedback + artificial conduction Delicate balance between heating and cooling processes (Rasia+15) Correct thermal and chemo-dynamical structure of CC/NCC clusters! Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

8 ICM Radial Profiles Entropy and Iron profiles Pressure profiles PRESSURE PROFILES: CC/NCC DICHOTOMY Observations: CC clusters show higher central pressure than NCC (e.g. Arnaud+10, McDonald+14) AGN simulations: good agreement with observational data (Planelles et al., submitted) Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

9 Hydrostatic Equilibrium Gas density clumping factor Cool-coreness vs dynamical state HE deviations GAS DENSITY CLUMPIMG FACTOR (e.g. Nagai+11) Gas density clumping Increases with radius Lower in radiative runs AGN (e.g. Walker+12, Eckert+13) (Planelles et al., submitted) Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

10 Hydrostatic Equilibrium Gas density clumping factor Cool-coreness vs dynamical state HE deviations CLUMPING: COOL-CORENESS VS DYNAMICAL STATE CC/NCC: core thermal properties Regular/disturbed: global dynamical state Regular: Similar density clumping for CC and NCC clusters (Planelles et al., submitted) Disturbed systems show larger density clumping than regular clusters Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

11 Hydrostatic Equilibrium Gas density clumping factor Cool-coreness vs dynamical state HE deviations HE DEVIATIONS CC NCC Dynamics of the intra-cluster gas: Condition of hydrostatic equilibrium: (Biffi et al., submitted) Regular Disturbed Average HE deviation ~ 10-20% The level of HE clearly depends on the clusters global dynamical state but not on their cool-coreness Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12

12 Conclusions TO TAKE HOME DIANOGA simulations: Re-simulations of 29 Lagrangian regions using GADGET-3: NR, CSF, AGN AGN feedback + artificial thermal diffusion: Realistic effective description of the processes generating the CC/NCC dichotomy CC/NCC: differences in terms of ICM properties Regular/disturbed: differences in terms of clumping and HE deviations General conclusions: Baryon physics affects simulated cluster properties and, therefore, cluster masses Simulations have increased in complexity, resolution and physics included Simulations for precision cosmology: additional physics and higher resolutions Challenge: precise observations + accurate modelling better physical understanding Exciting future in Computational and Observational Cosmology! Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June /12