The Magneticum Simulations, from Galaxies to Galaxy Clusters

Transcription

1 The Magneticum Simulations, from Galaxies to Galaxy Clusters Klaus Dolag, Universitäts Sternwarte München Remus, Saro, Steinborn, Teklu (USM), Hirschmann (AIP), Petkova (C2PAP), Ragagni (LRZ)...

2 What we reached so far Increase of resolution elements in compleated cosmological simulations over time. Cooling + star-formation + SMBH treatment

3 The Simulations... Physics: cooling+sfr+winds Springel & Hernquist 2002/2003 Metals cooling Wiersma et al SNIa,SNII,AGB Tornatore et al. 2003/2006 BH+AGN feedback Springel & Di Matteo 2006 Fabjan et al Hirschmann et al Steinborn et al Thermal conduction 1/20th Spitzer Dolag et al Numerics: New Kernels: WC6 Dehnen et al Low visc. scheme mr/hr (time dep. alpha) Dolag et al uhr (high order grad.) Beck et al. 2015

4 The Magneticum Simulations z=0 2x ~ groups with M > 5x10 13 M z=2 ~ 100 massive clusters with M > 2x10 14 M z=2 2x4536 3

5 Largest Simulation (Box0/mr) z=0 gas 38 Mpc 380 Mpc stars 3800 Mpc 3.8 Mpc

6 Sub-resolution star-formation:

7 Chemical enrichment:

8 Sub-resolution SMBH-formation:

9 What can we do...

10 What can we do... AGN properties Talk: FM , (M. Hirschmann) Cluster + SZ Poster: FM.5.p13 Stellar properties Poster: S317.p34

11 Gas mass of halos

12 Presssure profiles of clusters

13 Cluster Cosmology and PLANCK... CMB powerspectrum allows to measure cosmology with extreme high precission! WMAP Planck SPT und ACT

14 Cluster Cosmology and PLANCK... SZ imprint of Cosmological Structures onto CMB CMB powerspectrum allows to measure cosmology with extreme high precission! WMAP Planck SPT und ACT

15 Cluster Cosmology and PLANCK... SZ imprint of Cosmological Structures onto CMB CMB powerspectrum allows to measure cosmology with extreme high precission! Counting Galaxy Clusters WMAP Planck SPT und ACT

16 Cluster Cosmology and PLANCK... SZ imprint of Cosmological Structures onto CMB CMB powerspectrum allows to measure cosmology with extreme high precission! Counting Galaxy Clusters WMAP Planck SPT und ACT SZ Powerspectrum

17 Cluster Cosmology and PLANCK... SZ imprint of Cosmological Structures onto CMB CMB powerspectrum allows to measure cosmology with extreme high precission! Counting Galaxy Clusters WMAP Planck SPT und ACT SZ Powerspectrum

18 Using Magneticum Pathfinder Bocquet et al. 2015

19 Using Magneticum Pathfinder Bocquet et al. 2015

20 Verifying with Magneticum

21 Verifying with Magneticum

22 Magneticum Pathfinder SZ Maps 8.8 x 8.8 degree lightcone up to z=5 Predicted (y) from map: 1.2x10-6 Reconstructed (y) from public PLANCK data: 5.4x10-8 < (y) < 2.2x10-6 (Khatri & Sumyaev 2015)

23 Magneticum Pathfinder SZ Maps 8.8 x 8.8 degree lightcone up to z=5 Predicted y map from Local Universe simulation

24 SZ power spektrum Local Universe simulations give important contribution! Bocquet 2015 Tinker 2008 Simulation

25 Intra cluster light cd Galaxy member Galaxies ICL

26 Intra cluster light Einasto profile Einasto profile Simulations: Dolag et al Obs (A119): Bender et al 2015 cd + ICL

27 From ICL to outer halos of galaxies Well covers the differences between outer halo density profiles observed in Milky Way and Andromeda. DM Stars Halos from to M o Remus et al., in prep

28 Morphology of galaxies

29 Dynamics of galaxies Stellar Angular Momentum Teklu et al Stellar mass

30 Dynamics of galaxies Circularity Spheroidals Disks Teklu et al. 2015

31 Dynamics of galaxies Halo Spin Spheroidals Disks Holds even for the DM only simulation! Teklu et al. 2015

32 Simulations vs. observations Spheroidals Simulations Observations Disks Simulations Observations Stellar Angular Momentum Stellar mass Teklu et al Stellar mass

33 Simulations vs. observations Simulations Disks Spheroidals GAMA Observations Remus et al. 2015

34 Simulations vs. observations Comparison to observations holds also for higher redshifts! Remus et al., in prep Observations Simulations (Spheroidals) de Sande et al. (2013) van Dokkum et al. (2009) Onodera et al. (2012) Toft et al. (2012). Newman et al. 2010

35 Black Hole properties 2.5 Mpc Steinborn et al. 2015

36 AGN properties (optical + X-ray) Hirschmann et al. 2014

37 AGN distribution Correlation function Same AGN luminosity cut then observers. Steinborn, in prep. Miyaji et al. 2010

38 Conclusions (general) 1) ICM: Clusters well reproduced pressure profiles, SZ powerspectrum, Cluster counts, no tension with CMB cosmology! 2) Galaxies: Dynamics well reproduced spin, morphologies, colors, mass-size relation 3) Black holes: Observations well reproduced mass functions, luminosity functions, correlation functions, AGN-host connections 4) Universality in outer halos from galaxies to clusters, not directly related to morphology, reflecting recent dynamical activity More into details (future) 1) Large volumes for Planck/eROSITA for the first time, hydro-dynamical simulations cover large volumes and enough physical processes 2) ICM/AGN constarain sub-grid models combination of observables from ICM, AGNs (and galaxies) start to constrain our sub-grid models