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
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 2016 2/12
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: 1024 3 DM particles, L box =1 h -1 Gpc Re-simulation of 29 Lagrangian regions centred in clusters with M vir 10 15 h -1 M (24) and M vir (1-7) 10 14 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 3 10 13 h -1 M 70 clusters with M vir 10 14 h -1 M Susana Planelles Meeting on Fundamental Cosmology Barcelona, 15th June 2016 3/12
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 2016 4/12
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 2016 5/12
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 2016 6/12
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 2016 7/12
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 2016 8/12
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 2016 9/12
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 2016 10/12
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 2016 11/12
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 2016 12/12