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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)