1. Contamination of the CMB Planck data by galactic polarized emissions L. Fauvet, J.F. Macίas-Pérez

2. 2 The CMB from WMAP to Planck Polarized foregrounds 3D model of the galaxy: optimization Contamination of the CMB data L.Fauvet, Bielefeld workshop, 09/24/2009

3. 3 The Planck satellite mission ESA mission launched the may 14th 2009 2 instruments : LFI : 33, 44 and 70 GHz HFI : 100, 143, 217, 353, 545 and 857 GHz sensitivity: ∆T ≈ 2 μK angular resolution : 5 arcmin measurement of the CMB in temperature and polarization measurement of foreground emissions L.Fauvet, Bielefeld workshop, 09/24/2009

4. 4 The CMB from WMAP to Planck EE TT L.Fauvet, Bielefeld workshop, 09/24/2009 [Planck Blue book]

5. 5 The CMB from WMAP to Planck [Hinshaw et al, 2009] L.Fauvet, Bielefeld workshop, 09/24/2009 I QU

6. 6 Foregrounds for the CMB observation instrumental noise dust synchrotron free-free galaxies SZ (cinetic) SZ (thermal) CMB synchrotron dominates at ν < 70 GHz thermal dust dominates at ν > 70 GHz L.Fauvet, Bielefeld workshop, 09/24/2009

7. 7 Galactic polarized emissions dust emission B ω helical electron synchrotron emission dust grain star light polarization synchrotron emission (408 MHz) [Haslam et al, 1982] thermal dust emission (353 GHz) [Finkbeiner et al, 1999] L.Fauvet, Bielefeld workshop, 09/24/2009

8. 8 physical model of polarized foreground emissions depends on: the shape of the galactic magnetic field : regular component : BSS or ASS free parameter : pitch angle [Han et al, 2006] non regular component [Han et al, 2004] free parameter: A turb halo component, free parameter : A halo the distribution of relativistic electrons, free parameter: h r, CRE lo [Page et al, 2007; Sun et al, 2008] the distribution of dust grains [Page et al, 2007; Paladini et al, 2007] 3D model of the Galaxy [Han et al, 2006] L.Fauvet, Bielefeld workshop, 23/06/2009

9. 9 integrating along the line of sight polarization fraction related to the cosmic ray energy dimension slope s : p s = 0.75 idem for thermal dust ◦ thermal dust emission p d : the polarization fraction = 0.1 [Ponthieu et al, 2005] with: ◦ synchrotron emission 3D model of the Galaxy extrapolation at various μ : β s extrapolation at various μ : β d L.Fauvet, Bielefeld workshop, 09/24/2009

10. 10 Optimization of the model comparison with preexisting data ◦ 408 MHz all-sky continuum survey [Haslam et al, 1982] ◦ WMAP 5 years data (NASA satellite currently in fly) 5 polarized channels between 33 and 94 GHz [Hinshaw et al,2009] optimisation of the synchrotron emission model ◦ ARCHEOPS (ballon experiment, flu in 2003) 1 polarized channel at 353 GHz [Benoît et al, 2003] optimisation of the thermal dust emission model L.Fauvet, Bielefeld workshop, 09/24/2009

11. 11 Galactic profiles : I Haslam data, BSS field for various A turb L.Fauvet, Bielefeld workshop, 09/24/2009

12. 12 Galactic profiles : WMAP 5 years data + synchrotron emission (from green to red) (BSS model of magnetic field and exponnential distribution of relativistic electrons) 23 GHz QU L.Fauvet, Bielefeld workshop, 09/24/2009

13. 13 Galactic profiles : 353 GHz galactic profiles for various values of the latitudes the ARCHEOPS data and our model of thermal dust emission (BSS model of magnetic field and exponnential distribution of dust grains) L.Fauvet, Bielefeld workshop, 09/24/2009 UQI

14. 14 for the synchrotron emission model A turb < 0.25 B reg p = - 20 ± 10 deg h r < 15 kpc β s = -3.3 ± 0.1 Best fit parameters for the dust thermal emission A turb < 0.25 B reg p = - 20 ± 10 deg L.Fauvet, Bielefeld workshop, 09/24/2009 A turb p(deg) A turb BSS regular field

15. 15 Pixel to pixel comparison I WMAP Q WMAP U WMAP I SYNC Q SYNC U SYNC 23 GHz L.Fauvet, Bielefeld workshop, 09/24/2009

16. 16 Power spectrum WMAP 3 years data (black) |b|> 0 deg synchrotron emission model for differents value of the pitch angle (green (-70 deg) to red (10 deg)). 23 GHz TTEEBB TETBEB L.Fauvet, Bielefeld workshop, 09/24/2009

17. 17 Pixel to pixel comparison I ARCH Q ARCH U ARCH I DUST Q DUST U DUST 353 GHz L.Fauvet, Bielefeld workshop, 09/24/2009

18. 18 Power spectrum ARCHEOPS data (black) |b|>0 deg thermal dust emission model (red) 353 GHz EEBB TETBEB L.Fauvet, Bielefeld workshop, 09/24/2009 TT

19. 19 Contamination on the CMB black: model of galactic emission for |b| > 15 deg red : simulation of CMB TETBEB EEBBTT 143 GHz L.Fauvet, Bielefeld workshop, 09/24/2009

20. 20 Conclusion the model is a physical model of the galaxy comparison to the main data does exist no details but global features are well reproduced used into the separation component models efficient to simulate the Planck data and estimate the contamination of the CMB L.Fauvet, Bielefeld workshop, 09/24/2009