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Contamination of the CMB Planck data by galactic polarized emissions

Contamination of the CMB Planck data by galactic polarized emissions. L. Fauvet , J.F. Mac ί as -Pérez. The CMB from WMAP to Planck Polarized foregrounds 3D model of the galaxy : optimization

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Contamination of the CMB Planck data by galactic polarized emissions

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  1. Contaminationofthe CMB Planck databygalacticpolarizedemissions L. Fauvet, J.F. Macίas-Pérez

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

  3. The Planck satellitemission •ESA mission launched the may 14th 2009 • 2 instruments : LFI : 33, 44and70 GHz HFI : 100, 143, 217, 353, 545 and 857 GHz •sensitivity: ∆T ≈ 2 μK • angular resolution : 5 arcmin •measurementofthe CMB in temperatureandpolarization •measurementofforegroundemissions L.Fauvet, Bielefeld workshop, 09/24/2009

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

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

  6. Foregroundsforthe CMB observation instrumental noise dust synchrotron free-free galaxies SZ (cinetic) SZ (thermal) CMB synchrotrondominatesatν< 70 GHz thermal dustdominatesatν> 70 GHz L.Fauvet, Bielefeld workshop, 09/24/2009

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

  8. 3D model oftheGalaxy 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: Aturb halo component, free parameter : Ahalo •the distribution of relativistic electrons , free parameter: hr, CRElo [Page et al, 2007; Sun et al, 2008] • the distribution of dust grains [Page et al, 2007; Paladini et al, 2007] [Han et al, 2006] L.Fauvet, Bielefeld workshop, 23/06/2009

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

  10. Optimization of the model comparisonwithpreexistingdata ◦ 408 MHz all-skycontinuumsurvey[Haslam et al, 1982] ◦ WMAP 5 yearsdata(NASA satellitecurrently in fly) 5 polarizedchannelsbetween 33 and 94 GHz [Hinshaw et al,2009] optimisationofthesynchrotronemissionmodel ◦ARCHEOPS(ballonexperiment, fluin 2003) 1 polarizedchannelat 353 GHz [Benoît et al, 2003] optimisationofthethermal dustemissionmodel L.Fauvet, Bielefeld workshop, 09/24/2009

  11. Galacticprofiles : I Haslamdata, BSS fieldforvariousAturb L.Fauvet, Bielefeld workshop, 09/24/2009

  12. Galacticprofiles : 23 GHz Q U WMAP 5 yearsdata+ synchrotronemission(fromgreentored) (BSS model ofmagneticfieldandexponnentialdistributionofrelativisticelectrons) L.Fauvet, Bielefeld workshop, 09/24/2009

  13. Galacticprofiles : 353 GHz I Q U galacticprofilesforvariousvaluesofthelatitudestheARCHEOPS dataandour model of thermal dustemission (BSS model ofmagneticfieldandexponnentialdistributionofdustgrains) L.Fauvet, Bielefeld workshop, 09/24/2009

  14. Best fit parameters BSS regular field •forthesynchrotronemission model Aturb < 0.25 Breg p = - 20 ± 10 deg hr < 15 kpc βs= -3.3 ± 0.1 •forthedust thermal emission Aturb< 0.25 Breg p = - 20 ± 10 deg Aturb p(deg) Aturb p(deg) L.Fauvet, Bielefeld workshop, 09/24/2009

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

  16. Power spectrum 23 GHz TT EE BB TE TB EB WMAP 3 yearsdata(black) |b|> 0 deg synchrotronemission model fordifferentsvalueofthepitch angle (green (-70 deg) tored (10 deg)). L.Fauvet, Bielefeld workshop, 09/24/2009

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

  18. Power spectrum 353 GHz TT EE BB TE TB EB ARCHEOPSdata(black) |b|>0 deg thermal dustemission model (red) L.Fauvet, Bielefeld workshop, 09/24/2009

  19. Contamination on the CMB 143 GHz TT EE BB TE TB EB black: model ofgalacticemissionfor|b| > 15 deg red : simulationof CMB L.Fauvet, Bielefeld workshop, 09/24/2009

  20. Conclusion • the model is a physical model ofthegalaxy •comparisontothemaindatadoesexist •nodetails but global featuresare well reproduced •usedintotheseparationcomponentmodels •efficienttosimulatethe Planck dataandestimatethecontaminationofthe CMB L.Fauvet, Bielefeld workshop, 09/24/2009

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