1 / 20

A self-similar study of SZ cluster number counts from X-ray properties

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

chibale
Download Presentation

A self-similar study of SZ cluster number counts from X-ray properties

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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

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

  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 (Ωm,σ8...)

  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 (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 Lseuil ⇒ V(L<Lseuil)=0 Evolution of L-T

  9. 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

  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) (Vauclair et al.2003)

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

  17. 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

  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

More Related