M.D., Beijing, August 2006 1

Coherent analysis of Coherent analysis of CMB anisotropiesCMB anisotropiesCMB, structures and ForegroundsCMB, structures and Foregrounds

Marian Douspis

Nabila Aghanim, Mathieu Langer

(IAS - Orsay)

Douspis, Aghanim & Langer A&A, 2006

M.D., Beijing, August 2006 2

ObservationsObservations Power spectrum of

temperatureanisotropies

Power excess Power excess @ small scales @ small scales compared tocompared to

primary CMBprimary CMB

M.D., Beijing, August 2006 3

Micro-Waves SkyMicro-Waves Sky Primary Anisotropies (CMB)

Secondary Anisotropies (SZ [Thermal])

Extra-galactic sources (IR, radio)

Galactic Emissions

Released data are “cleaned” from galactic and extra-galactic signal (resolved sources)

1st hypothesis: Excess = SZ effect

M.D., Beijing, August 2006 4

Previous worksPrevious works Fix cosmology (CP) with signal @ Choose a SZ spectrum (from one simulation) Add primary CMB and £ SZ() Ampl. given by fit of signal @ Deduce the SZ contribution @ (Bond et al., Goldstein et al., Kuo et al., Redhead et al., wmap3)

Ignores the inherent link between SZ spectrum and cosmological parameters

Need coherent analyse to estimate the SZ contrib.

M.D., Beijing, August 2006 5

Computation of the SZ spectrumComputation of the SZ spectrum

C.P. appear in the computation of the SZ spectrum

SZ emission of a single cluster for a hot gas distribution in a NFW profile of DM Choose a mass function (Jenkins) to compute the cluster number counts on the sky (dn/dM) Integrate over the sky (Komatsu & Seljak)

M.D., Beijing, August 2006 6

SZ SpectrumSZ Spectrum

(WMAP 1st year)

M.D., Beijing, August 2006 7

SZ Contribution 1/2SZ Contribution 1/2

8 high , n high

degeneracies

Need for a coherent analysis

M.D., Beijing, August 2006 8

SZ Contribution 2/2SZ Contribution 2/2

Any room for an additional contribution ?

1st coherent determination of the SZ contribution

M.D., Beijing, August 2006 9

Residual Point SourcesResidual Point Sources

In each experiment (@small scales)some contributions from unresolved point sources(IR/radio) with Flux Detection threshold remain

Model: (poissonian distribution) to be added to CMB+SZ spectra (Bi

are new free parameters in the fit)

M.D., Beijing, August 2006 10

Residual point sources Residual point sources spectrumspectrum

1 contribution/spectrum of source by experiment

M.D., Beijing, August 2006 11

Point sources Point sources contribution 1/3contribution 1/3

Including SZ and PS:Cosmology in

agreement with concordance model

obtained at large scales

l<1500l<10000

M.D., Beijing, August 2006 12

SZ(150) ~ 5 %PS(acbar)~ 35%

SZ(30) ~ 10 %PS(cbi) ~ 40%

SZ(30) ~ 15 %PS(bima)~ 5%

@l=2000

Point sources Point sources contribution 2/3contribution 2/3

M.D., Beijing, August 2006 13

Comparison with point sources studies?

Agreement with: Toffolatti et al.

If PS contribution supposed ?:

cosmology OK

Contribution sources Contribution sources ponctuelles 3/3ponctuelles 3/3

M.D., Beijing, August 2006 14

ConclusionsConclusions

Tools developped for a coherent approach of the CMB and LSS

(Primary/secondaries/extragalactic sources) Determination of SZ and PS contributions as a function of for each experiment (8, B

i ) Analysis needed for future data analysis (better error bars, intercalibration) Improvements needed as well (running, lensing, dependency in cluster )

M.D., Beijing, August 2006 15

Thank you for your attention

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