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Simulating the SZ Sky
Predictions for Upcoming Sunyaev-Zel’dovich Effect
Galaxy Cluster Surveys
Eric J. Hallman
CASA, University of Colorado
16 February, 2007
Clusters of Galaxies as Cosmological Probes Conference
Aspen, CO
Collaborators
• Brian O’Shea (LANL)
• Jack Burns (University of Colorado)
• Mike Norman (UCSD)
• Rick Wagner (UCSD)
• Robert Harkness (SDSC)
SZ Surveys of Galaxy Clusters
• Survey yield depends on cosmology AND gas physics AND details of dynamical states of clusters
• How does observable scale with mass?
• What is the selection function in mass for cluster surveys?
• Also depends on instrument properties, survey strategy, confusion, etc.
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•ΛCDM m=0.3, =0.7, 8=0.9•AMR gives high resolution (8 h-1 kpc) in dense regions• 512 h-1 Mpc on a side, use 7 levels of refinement• 5123 root grid, 7 levels everywhere•DM mass = 7.3x1010 Msolar, baryon mass = 1.1x1010
•Initial run is adiabatic physics only
Adaptive Mesh Refinement (AMR) Light Cone Simulations (N-body + Hydro)
Enzo (O’Shea et al. 2005, http://cosmos.ucsd.edu/enzo)
How do we make simulated surveys?
• Surveys sample the universe at all observable epochs, so….
• Stack simulations at different evolutionary states in discrete redshift intervals to approximate
• Each z uses physical extent of box in line of sight which matches that redshift interval
• Modify angular scale of image to fixed angular size for all redshifts, flux diminishes (but not in SZE!)
• Random shifting, rotating, some tiling• Model telescope response, background, foreground
contamination, point sources, etc etc (Future work)
Sky Surveys
• X-ray and SZE synthetic surveys• 5000+ Clusters above 1x1014Msolar in field out to z=3• 2048x2048, 10x10 degrees, 17.6” / pixel
Why do we have N-body + hydro?
• In real universe, clusters are neither isothermal nor in equilibrium generally (e.g. M. Voit’s talk)
• Variations in cluster physics make a difference (Evrard’s and Rudd’s talks)
• In order to characterize scatter, survey selection (in mass) from simulations, must include baryons!
Cold Fronts Filaments Bullet Subcluster
1E 0657-56Abell 1795Abell 2256
(Sun et al 2002) (Fabian et al 2001) (Markevitch et al 2002)
Clusters are NOT generally in equilibrium (dynamical, hydrostatic or otherwise)
Merger Boosting
• See also C. Sarazin’s talk
Identification of Sources
• Hallman et al. 2007
Identification with SExtractor
• Upcoming Surveys:
SPT: 1.0’, ~4000deg^2, 10K
APEX-SZ: 1.0’, ?deg^2, 10K
ACT: 1.7’,100-200deg^2,2K
Planck, 5.0’, all-sky, 2.2K
• 90% limits for 200 stacking realizations of the survey
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• APEX: 472 +- 100
• ACT: 1211+- 200
• Planck: 90 +- 40
What else should be included?
• What we get: full array of dynamical stateslarge volumegaussian background
• What we’re missing (so far) ref. N. Sehgalatmospherepoint sourcesadditional physicsother instrumental effects We are working on all of these!
Halos in the Simulation
• Identify via HOP algorithm
• 12000 clusters at z=0 in simulation box above M = 5x1013Msolar
• Identify their locations in the 2d projection of the simulated survey
• Match to locations of halos provided by SExtractor
• Hallman et al. 2007
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Recall L. Verde’s talk
Stacking Caveats
• Stacking with a single simulation has problems
• Constant physical resolution (as f(z)) on the grid does not equal constant angular resolution on the sky
• Large scale correlations can be generated
• How can we solve that? Use multiple simulations!
The Big One(s)
• We are generating a complete, unique numerical simulation for each z
• Each simulation has a physical size specified by it’s angular extent at that redshift (ITC 10 degrees square).
• Allows lower computational effort for the most nearby volumes, since their physical resolution must be highest.
• Eliminates stacking issues (almost).• 2 cubic Gpc of total simulated volume
Plans for Huge LCs
• From smaller set of simulations, refine baryonic physics (cooling, star formation, SN feedback, AGN feedback, conduction, etc.)
• Vary cosmology (e.g., w, 8), determine precision necessary to distinguish
• Synthetic Observations (X-ray/SZE primarily) including both instrumental effects, backgrounds/foregrounds, etc.
Summary
• Survey yields depend on luminosity function, which depends on cosmology AND detailed baryonic physics AND dynamical states AND confusion, etc.
• If you want high precision, non-trivial problems in counting clusters
• Numerical N-body + hydro (!) simulations coupled with realistic synthetic observations allow us to understand systematics, get the “right” answer!
Sample Stacking Solution
Synthetic Observations
Constraints from Clusters, Dark Energy Equation of State
• Haiman et al 2001
Results from Adiabatic Physics Model (Projected Emission-Weighted Temperature)
5 Mpc