1 studying clusters and cosmology with chandra licia verde princeton university some thoughts…
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Studying clusters and cosmology
with Chandra
Licia VerdeLicia Verde Princeton University
Some thoughts…
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Overview
•The potential of combining: X-rays + optical + CMB…..
•Clusters scaling relations with X-rays and the Sunyaev-Zeldovich effect
• constraining dark energy (Quintessence) •Conclusions
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Coordinated Cluster Measurements
X-ray Flux: • Temperature and luminosity probe
mass
mm-Wave: • SZ – Compton Scattering
Optical: • Redshift velocity dispersion• Photometry and lensing
Galaxy Cluster
HOT Electrons chandra
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SZ SignatureHot electron gas imposes a unique spectral signature
NO SZ Contribution in Central Band
145 GHzdecrement
220 GHznull
270 GHzincrement
1.4°x 1.4°Easy to find!
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Multiple uses• Standard candles
• Standard rulers
• Probes of volume
• Probes of velocity field
• Probes of initial conditions
Clusters as Cosmological Probes
Multiple observables
• Clusters counts (*)
• SZ luminosity
• Central SZ decrement
• X-ray temperature (*)
• X-ray luminosity(*)
• Angular size(*)
• Velocity Dispersion
• Redshift
• Lensing Mass
• Kinetic SZ amplitude
Linked theoretical/observational effort essential for using these observables as cosmological probes.
• Amplitude of fluctuations
• Scaling relations
• Gravitational lensing of CMB gives
• Kinetic SZ gives v2
• Cluster counts give– N(M,z)
– N(FSZ,z)
Need to know cluster physics
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Clusters scaling relationsClusters scaling relations
Mohr et al 1997, Mohr et al 2000
(e.g., size temperature, mass-temperature)
(Verde et al. 2000)
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New scaling relations that include the SZ decrementNew scaling relations that include the SZ decrement
Observables: SZ, angular size, redshift,Temperature
“constraints”: M-T relation /1)1( MzT f
)1,5.1(
Virial relation MTR
Total SZ decrement22
Ad
TMS
(Verde, Haiman, Spergel 2002)chandra
THSC
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If our understanding of cluster physics is correct
Clusters should occupy a fundamental plane
Narrow
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Different cluster physics and/or cosmology
Modifications in the Position, orientation and redshift evolution of the planeScaling relations with SZ
narrow broad
(THSC prediction)
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Formation redshift?Formation redshift?
Only formation redshift Only stochastic
Mathiessen 2001 finds no evidence for zf being relevant to clusters properties
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2D KS test
fM Lacey & Cole 94 parameter for the formation redshift distribution
Assume cosmology, study cluster physics
300 clusters with follow up
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/1)1( MzT fBack to: )1,5.1(
Observations e.g., Xu et al. 2001, Mohr, Evrard 1997, Mohr et al 1999
98.16.1
Effect of formation redshift 6.1eff
Deviations from virialization parameterized by
Can constrain a fiducial model:05.01.05.1
03.01For a fiducial model
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Assume formation redshift distribution is importantConstraints from zSz ,,Used KS, Lokelihood is much more sensitive
Assume cluster physics, study cosmology
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MAP 2 yr
Clusterabundance
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ADD information about dN/dz (mass function)
Break the cluster physics/cosmology degeneracy
With Z. Haiman
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Shown a “taste” of the many possibilites
The fundamental plane/scaling relations approach can be generalized to include other observables such as velocity dispersion, X-ray luminosity, shear, central SZ decrement….
Used KS test, likelihood is much more sensitive
Insensitive to the mass function and independent from it
Can be used in tandem with dN/dz (clusters counts) to lift degeneracies between cosmology and cluster physics
Important to constrain clusters physics (fixed cosmology)
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Perlmutter et al. 1998
deBernardis et al. 2001
Verde et al 2002
Nature? Equation of state?
Dark energy Dark energy
From Verde et al. 2002
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MAP will constrain and cosmological parameters
The growth of structure (i.e. cluster abundance evolution)
Nature ofdark energy
(once we know clusters physics)
Haiman et al. 2000
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• X-ray +CMB +optical + theory
• Clusters scaling relations with SZ (Tx) (study cluster physics and cosmology)
• constrain dark energy exploiting growth rate of structure
Conclusions
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