1. 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

2. ➢ Modeling the clusters population ➢ X-ray results ➢ Prediction on SZ number counts ➢ Conclusion Outline

3. Modeling Clusters population Need mass Population very sensitive to the mass & growth factor Modeling by mass function (Press & Schechter 1974) Dependent of the cosmology (Ω m,σ 8...)

4. 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...

5. Modeling Clusters population The Temperature function (1) ➢ From the mass function ➢ From the observations

6. X-ray results The samples Namez Temperature (keV) Number BAX0 → 0.11 → 965 400deg 2 deep0.35 → 0.92 → 1136 MACS 20070.5 → 0.77 → 1212 MACS 20100.3 → 0.454.7 → 1434 (See Viklhinin et al.2009, Ebeling et al.2007, Ebeling et al.2010 & http://bax.ast.obs-mip.fr)

7. X-ray results Observational temperature function

8. X-ray results Volume corrections L seuil ⇒ V(L<L seuil )=0 Evolution of L-T

9. X-ray results MCMC analysis 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.) ➢ COSMOMC package (Lewis & Briddle 2002) Constraints on Ω m, Ω Λ, σ 8, h... & A TM

10. X-ray results Without clusters

11. X-ray results First attempt : MCMC Result

12. X-ray results First Attempt (suite)

13. X-ray results First Attempt (suite) Comparing the mass functions Values from MCMC chains

14. X-ray results First Attempt (suite)

15. X-ray results T-M redshift evolution (Vauclair et al.2003)

16. X-ray results T-M redshift evolution Using all samples

17. X-ray results T-M redshift evolution A TM =8.24keV α= -0.62 A TM =8.4keV α= -0.62 A TM =8.28keV α= -0.61

18. 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)

19. SZ number counts Predictions (Delsart, Barbosa & Blanchard 2010)

20. 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