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Coherent analysis of CMB anisotropies CMB, structures and Foregrounds. Marian Douspis Nabila Aghanim, Mathieu Langer (IAS - Orsay). Douspis, Aghanim & Langer A&A, 2006. Observations. Power spectrum of temperature anisotropies. Power excess @ small scales compared to primary CMB. - PowerPoint PPT Presentation
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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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