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1 Studying clusters and cosmology with Chandra Licia Verde Princeton University Some thoughts…
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2 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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3 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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4 SZ Signature Hot electron gas imposes a unique spectral signature NO SZ Contribution in Central Band 145 GHz decrement 220 GHz null 270 GHz increment 1.4 ° x 1.4 ° Easy to find!
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5 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 v 2 Cluster counts give –N(M,z) –N(F SZ,z) Need to know cluster physics
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6 Clusters scaling relations Mohr et al 1997, Mohr et al 2000 (e.g., size temperature, mass-temperature) (Verde et al. 2000)
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7 New scaling relations that include the SZ decrement Observables: SZ, angular size, redshift,Temperature “ constraints”: M-T relation Virial relation Total SZ decrement (Verde, Haiman, Spergel 2002) chandra THSC
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8 If our understanding of cluster physics is correct Clusters should occupy a fundamental plane Narrow
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9 Different cluster physics and/or cosmology Modifications in the Position, orientation and redshift evolution of the plane Scaling relations with SZ narrow broad (THSC prediction)
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10 Formation redshift? Only formation redshiftOnly stochastic Mathiessen 2001 finds no evidence for zf being relevant to clusters properties
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11 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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12 Back to: Observations e.g., Xu et al. 2001, Mohr, Evrard 1997, Mohr et al 1999 Effect of formation redshift Deviations from virialization parameterized by Can constrain a fiducial model: For a fiducial model
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13 Assume formation redshift distribution is important Constraints from Used KS, Lokelihood is much more sensitive Assume cluster physics, study cosmology
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14 MAP 2 yr Cluster abundance
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15 ADD information about dN/dz (mass function) Break the cluster physics/cosmology degeneracy With Z. Haiman
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16 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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17 Perlmutter et al. 1998 deBernardis et al. 2001 Verde et al 2002 Nature? Equation of state? Dark energy From Verde et al. 2002
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18 MAP will constrain and cosmological parameters The growth of structure (i.e. cluster abundance evolution) Nature of dark energy (once we know clusters physics) Haiman et al. 2000
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19 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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20 END
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