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A self-similar study of SZ cluster number counts from X-ray properties. Pierre Delsart 1 , Alain Blanchard 1 , Domingos Barbosa 2 1 IRAP, Toulouse, France 2 Instituto de Telecomunicaçoes, Aveiro, Portugal X-ray Universe, Berlin, 30th June 2011. Outline. ➢ Modeling the clusters population
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A self-similar study of SZ cluster number counts from X-ray properties • Pierre Delsart1, Alain Blanchard1, Domingos Barbosa2 • 1IRAP, Toulouse, France • 2Instituto de Telecomunicaçoes, Aveiro, Portugal • X-ray Universe, Berlin, 30th June 2011
Outline ➢ Modeling the clusters population ➢ X-ray results ➢ Prediction on SZ number counts ➢ Conclusion
Modeling Clusters population Need mass Population very sensitive to the mass & growth factor Modeling by mass function (Press & Schechter 1974) Dependent of the cosmology (Ωm,σ8...)
Modeling Clusters population The T-M scaling relation Mass not measurable Needs : True observable (luminosity, temperature...) Observable-mass relation (Kaiser 1991) Energy conservation, thermalization, isothermal sphere...
Modeling Clusters population The Temperature function (1) ➢ From the mass function ➢ From the observations
X-ray results The samples (See Viklhinin et al.2009, Ebeling et al.2007, Ebeling et al.2010 & http://bax.ast.obs-mip.fr)
X-ray results Observational temperature function
X-ray results Volume corrections Lseuil ⇒ V(L<Lseuil)=0 Evolution of L-T
X-ray results MCMC analysis ➢ COSMOMC package (Lewis & Briddle 2002) CMB from WMAP 7 years (Jarosik et al.2010) SNIa from SDSS, LOWZ, ESSENCE, HST (Kessler et al.2010) Galaxy power spectrum from SDSS DR7 (Reid et al.2010) X-ray temperature function (Delsart & Blanchard in prep.) Constraints on Ωm, ΩΛ, σ8, h... & ATM
X-ray results Without clusters
X-ray results First attempt : MCMC Result
X-ray results First Attempt (suite)
X-ray results First Attempt (suite) Comparing the mass functions Values from MCMC chains
X-ray results First Attempt (suite)
X-ray results T-M redshift evolution (Vauclair et al.2003) (Vauclair et al.2003)
X-ray results T-M redshift evolution Using all samples
X-ray results T-M redshift evolution ATM=8.24keV α= -0.62 ATM=8.4keV α= -0.62 ATM=8.28keV α= -0.61
SZ number counts SZ effect & scaling relation ➢Inverse Compton scattering ➢CMB blackbody spectrum distorsion Surface brightness (see Barbosa et al.1996; Delsart, Barbosa & Blanchard 2010)
SZ number counts Predictions (Delsart, Barbosa & Blanchard 2010)
Conclusion ■ Clusters as cosmological test need to be well understood ■Constraints on the clusters inner properties ■Redshift evolution in T-M scaling law must evolve. ■Consistency between independant samples ■Lower SZ number counts than expected