NiFTy2014Cluster Comparison

Magneticum Pathfinder Simulations

Klaus DolaLuca TornatoreMichaela HirschmannJoe MohrStefano BorganiGiuseppe MuranteAndi BurkertHans Böhringer

Gabriella De LuciaMassimo MeneghettiMatteo VielVeronica BiffiRhea RemusDunja FabianEdoardo Tescari+++

Klaus Dolag 99.9%Luca TornatoreMichaela HirschmannJoe MohrStefano BorganiGiuseppe MuranteAndi BurkertHans Böhringer

The Aim

Cosmological, hydrodynamical simulations which at the sametime allows predictions for ICM and stellar component forongoing/future missions.

The Aim

Mock optical/x-ray/SZE observations using SkyLens (Meneghetti 2010), X-Mass (Rasia 2007) and Phox (Biffi 2011), Liu et al. (2014, in prep).

z= 0

DM simulation (M,M−XXL)72 byte per DM particleHydrosimulationca. 800 byte per DM particle

Data management Up to 20TB per snap!!• Sub­find output• Information Block• Peano­Hilbert Key index files (DM, gas, stars, BHs)

Including:

●TreePM­SPH code P­GADGET3 (Springel 2005).●Entropy­conserving formulation of SPH (Springel & Hernquist 2002).●Higher order kernel based on the bias­corrected, sixth­order Wendland kernel (Dehnen & 

Aly 2012) + 295 neighbours●Low viscosity scheme to track turbulence (Dolag et al. 2005)● Isotropic thermal conduction with 1/20 Spitzer (Dolag et al. 2004).●Cooling + star formation + winds (Springel & Hernquist 2002/2003) with v = 350 km/s●Metals, Stellar population and chemical enrichment, SN­Ia, SN­II, AGB (Tornatore et al. 

2003/2006)●Cooling tables (Wiersma et al. 2009)●BH and AGN feedback (Springel & Di Matteo 2006, Fabjan et al. 2010) radio/quasar 

mode + modifications (Hirschmann+13):●BHs seeded from FoF on Star Particles (smaller linking length of 0.05 of mean DM 

separation) hr M*­›1010M

⊙/h 

●  BH are not pinned to most bound particles:●Forced momentum conservation for the smooth gas accretion without momentum 

transfer when swallowing ●Conservation of momentum and centre of mass for BHs merging

●Dynamical friction force for low resolution sims (Chandrasekhar 1943) from properties of hosting SubHalo (updated on the fly)

Magneticum Pathfinder

Add ons:

● On the fly Sub­Find Springel et al. 2001/2010, Dolag et al. 2009

● Photometric code to assign optical/near­IR luminosities to galaxies (u,V,G,r,i,z,Y,J,H,K,L,M) Saro et al. 2006, Nuzza et al. 2010

● On the fly Cluster/Groups properties

● Novel sub­data access scheme allowing an efficient read­out of particles belonging to a galaxy cluster

Reading particles for most massive object

Fast Data Access

25 Mpc

Mass Function

Boquet et al. (2014, in prep)

Lightcones13 x 13 de g

rees

Deep (z~2) 13x13 degrees (z~5) 8x8 degrees lightcones

Lightcones13 x 13 de g

rees

13 x 13 de g

ree

High-z clusters &protoclusters

Deep (z~2) 13x13 degrees (z~5) 8x8 degrees lightcones

Lightcones

X-ray

Post-processing already finished forX-ray and SZE mock sky

Lightcones

Post-processing already finished forX-ray and SZE mock sky

Liu et al. (2014, in prep)

Lightcones

Post-processing already finished forX-ray and SZE mock sky

13 x 13 degree

tSZMock SPT fields

Noise: 18 μk arcmin-1

FHWM: 1.1 arcminNoise: 44 μk arcmin-1

FHWM: 1.6 arcmin

Killedar+14, in preparation

First Results

Already used in: 

McDonald,  M.  +  SPT  team  2014,  arXiv1404.6250;  Hirschmann,  M., Dolag, K., Saro, A., Borgani, S., Burkert, A. 2013, arXiv1312.2462; Saro, A. + SPT team 2013, MNRAS 428, 1395; Biffi, V., Dolag, K., Boehringer, H. 2013, MNRAS 436, 460; Wu, H­Y., Hahn, O., Evrard, A.E., Wechsler, R.H., Dolag, K. 2013, MNRAS 436, 460; Planck Collaboration 2013, A&A 550, 131; Remus, R­S., Burkert, A., Dolag, K., Johansson, P.H., Naab, T., Oser,  L.,  Thomas,  J.  2013,  ApJ  766,  71;  Iannuzzi,  F.,  Dolag,  K.  2012, MNRAS 427, 1024

Galaxies/AGNs

Stellar Mass Function (Hirschmann+14)

Galaxies/AGNs

AGN Luminosity Function (Hirschmann+14)

AGN Luminosity Function radio to X-ray(Hirschmann+14)

Weinmann et al. 2010

Galaxy population

Downsizing in specific star formation rate

Clusters/ICM

L-T relation

Pressure profiles

Liu et al., in preparation

Conclusions

Magneticum Pathfinder Simulations is a set of cosmological,hydrodynamical simulations which at the same time allows predictionsfor ICM, IGM and stellar and AGN component especially designed tofully exploit ongoing/future multiwavelenght missionsfully exploit ongoing/future multiwavelenght missions.• Simulated stellar properties (reasonable)luminosity function, colors, specific star-formation rates

• ICM properties (very good, e.g Biffi et al.+13)pressure profiles, x-ray scaling relations

• AGN properties (very good) (Hirschmann et al. 2014)accretion histories, luminosity functions

• Deep light-conesimportant for outskirts, cluster finding, other side projects

• Multi purpose X-ray/SZE simulator available(Biffi et al. 2011, Liu et al. 2014)