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

Pierre Delsart1, Alain Blanchard1, Domingos Barbosa2

1IRAP, Toulouse, France2Instituto de Telecomunicaçoes, Aveiro, Portugal

X-ray Universe, Berlin, 30th June 2011

➢ Modeling the clusters population

➢ X-ray results

➢ Prediction on SZ number counts

➢ Conclusion

Outline

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 populationThe T-M scaling relation

Mass not measurable

Needs : True observable (luminosity,

temperature...)Observable-mass relation (Kaiser 1991)

Energy conservation, thermalization, isothermal sphere...

Modeling Clusters populationThe Temperature function (1)

➢ From the mass function

➢ From the observations

X-ray results

The samples

Name zTemperatur

e (keV)Number

BAX 0 → 0.1 1 → 9 65

400deg2 deep

0.35 → 0.9 2 → 11 36

MACS 2007 0.5 → 0.7 7 → 12 12

MACS 2010 0.3 → 0.45 4.7 → 14 34

(See Viklhinin et al.2009, Ebeling et al.2007, Ebeling et al.2010 & http://bax.ast.obs-mip.fr)

X-ray resultsObservational temperature function

X-ray results

Volume corrections

Lseuil ⇒ V(L<Lseuil)=0

Evolution of L-T

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 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=8.24keVα= -0.62

ATM=8.4keVα= -0.62

ATM=8.28keVα= -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