Contamination of the CMB Planck data by galactic polarized emissions
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Contamination of the CMB Planck data by galactic polarized emissions L. Fauvet, J.F. Macίas- Pérez
description
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 - PowerPoint PPT Presentation
Transcript of Contamination of the CMB Planck data by galactic polarized emissions
Contamination of the CMB Planck data by galactic polarized
emissions
L. Fauvet, J.F. Macίas-Pérez
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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
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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
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The CMB from WMAP to Planck
EE
TT
L.Fauvet, Bielefeld workshop, 09/24/2009[Planck Blue book]
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The CMB from WMAP to Planck
[Hinshaw et al, 2009]
L.Fauvet, Bielefeld workshop, 09/24/2009
I
Q U
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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 GHzL.Fauvet, Bielefeld workshop, 09/24/2009
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Galactic polarized emissions
dust emission
Bω
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]
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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]
3D model of the Galaxy
[Han et al, 2006]
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• integrating along the line of sight
polarization fraction related to the cosmic ray energy dimension slope s : ps = 0.75
idem for thermal dust
◦ thermal dust emission
pd : the polarization fraction = 0.1 [Ponthieu et al, 2005]
with:
◦ synchrotron emission
3D model of the Galaxy
• extrapolation at various μ : βs
• extrapolation at various μ : βd
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Optimization of the modelcomparison 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
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Galactic profiles : I
Haslam data,BSS field for various Aturb
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Galactic profiles :
WMAP 5 years data + synchrotron emission (from green to red) (BSS model of magnetic field and exponnential distribution of relativistic electrons)
23 GHzQ U
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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
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• for the synchrotron emission model
Aturb < 0.25 Breg p = - 20 ± 10 deg hr < 15 kpc βs = -3.3 ± 0.1
Best fit parameters• for the dust thermal emission
Aturb < 0.25 Breg
p = - 20 ± 10 deg
L.Fauvet, Bielefeld workshop, 09/24/2009
Aturb p(deg)
p(de
g)A t
urb
BSS regular field
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Pixel to pixel comparison I WMAP
Q WMAP
U WMAP
I SYNC
Q SYNC
U SYNC
23 GHz
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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 GHzTT EE BB
TE TB EB
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Pixel to pixel comparison I ARCH
Q ARCH
U ARCH
I DUST
Q DUST
U DUST
353 GHz
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Power spectrum
ARCHEOPS data (black) |b|>0 deg thermal dust emission model (red)
353 GHzEE BB
TE TB EB
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TT
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Contamination on the CMB
black: model of galactic emission for |b| > 15 degred : simulation of CMB
TE TB EB
EE BBTT 143 GHz
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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
