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Coherent analysis of CMB anisotropies CMB, structures and Foregrounds

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.

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Coherent analysis of CMB anisotropies CMB, structures and Foregrounds

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  1. Coherent analysis of CMB anisotropiesCMB, structures and Foregrounds Marian Douspis Nabila Aghanim, Mathieu Langer (IAS - Orsay) Douspis, Aghanim & Langer A&A, 2006

  2. Observations Power spectrum of temperature anisotropies Power excess @ small scales compared to primary CMB

  3. Micro-Waves Sky • Primary Anisotropies (CMB) • Secondary Anisotropies (SZ [Thermal]) • Extra-galactic sources (IR, radio) • GalacticEmissions Released data are “cleaned” from galactic and extra-galactic signal (resolved sources) 1st hypothesis: Excess = SZ effect

  4. Previous works • Fix cosmology (CP) with signal @ • Choose a SZ spectrum (from one simulation) • Add primary CMB and £ SZ(n) • 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.

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

  6. SZ Spectrum (WMAP 1st year)

  7. SZ Contribution 1/2 8 high , n high degeneracies Need for a coherent analysis

  8. SZ Contribution 2/2 Any room for an additional contribution ? 1st coherent determination of the SZ contribution

  9. Residual 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)

  10. Residual point sources spectrum 1 contribution/spectrum of source by experiment

  11. Point sources contribution 1/3 Including SZ and PS: Cosmology in agreement with concordance model obtained at large scales l<1500 l<10000

  12. Point sources contribution 2/3 SZ(30) ~ 10 % PS(cbi) ~ 40% SZ(150) ~ 5 % PS(acbar)~ 35% SZ(30) ~ 15 % PS(bima)~ 5% @l=2000

  13. Contribution sources ponctuelles 3/3 Comparison with point sources studies? Agreement with: Toffolatti et al. If PS contribution supposed ?: cosmology OK

  14. Conclusions • 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 (s8, Bni ) • Analysis needed for future data analysis (better error bars, intercalibration) • Improvements needed as well (running, lensing, dependency in cluster f)

  15. Thank you for your attention & Thank you for your invitation

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