Loading in 5 sec....

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

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

Download Presentation

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

Loading in 2 Seconds...

- 71 Views
- Uploaded on
- Presentation posted in: General

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

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.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

- 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