A self-similar study of SZ cluster number counts from X-ray properties Pierre Delsart 1, Alain...
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![Page 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.](https://reader035.fdocuments.in/reader035/viewer/2022070413/5697bfe01a28abf838cb35b4/html5/thumbnails/1.jpg)
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
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➢ Modeling the clusters population
➢ X-ray results
➢ Prediction on SZ number counts
➢ Conclusion
Outline
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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...)
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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...
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Modeling Clusters populationThe Temperature function (1)
➢ From the mass function
➢ From the observations
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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)
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X-ray resultsObservational temperature function
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X-ray results
Volume corrections
Lseuil ⇒ V(L<Lseuil)=0
Evolution of L-T
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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
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X-ray results
Without clusters
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X-ray results
First attempt : MCMC Result
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X-ray results
First Attempt (suite)
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X-ray results
First Attempt (suite)
Comparing the mass functions
Values from MCMC chains
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X-ray results
First Attempt (suite)
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X-ray results
T-M redshift evolution
(Vauclair et al.2003)(Vauclair et al.2003)
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X-ray results
T-M redshift evolution
Using all samples
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X-ray results
T-M redshift evolution
ATM=8.24keVα= -0.62
ATM=8.4keVα= -0.62
ATM=8.28keVα= -0.61
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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)
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SZ number counts
Predictions
(Delsart, Barbosa & Blanchard 2010)
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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