Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops - Archive ouverte HAL Access content directly
Journal Articles Astronomy and Astrophysics - A&A Year : 2005

## Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops

M. Tristram
• Function : Author
A. Amblard
• Function : Author
R. Ansari
• Function : Author
J. Aumont
Alain Benoit
• Function : Author
J.-Ph. Bernard
• Function : Author
J.J. Bock
• Function : Author
F.R. Bouchet
A. Bourrachot
• Function : Author
P. Camus
• Function : Author
J.-F. Cardoso
F. Couchot
P. de Bernardis
• Function : Author
F.-X. Désert
• Function : Author
P. Fosalba
M. Giard
• Function : Author
R. Gispert
• Function : Author
J. Grain
• Function : Author
J.-C. Hamilton
S. Hanany
• Function : Author
S. Henrot-Versillé
Guilaine Lagache
A. E. Lange
• Function : Author
• Function : Author
B. Maffei
• Function : Author
S. Masi
• Function : Author
F. Mayet
F. Nati
G. Patanchon
• Function : Author
O. Perdereau
• Function : Author
Stéphane Plaszczynski
S. Prunet
J.-L. Puget
• Function : Author
C. Renault
• Function : Author
D. Santos
• Function : Author
D. Vibert
• Function : Author

#### Abstract

We present the first measurement of temperature and polarization angular power spectra of the diffuse emission of Galactic dust at 353 GHz as seen by Archeops on 20% of the sky. The temperature angular power spectrum is compatible with that provided by the extrapolation to 353 GHz of IRAS and DIRBE maps using \cite{fds} model number 8. For Galactic latitudes $|b| \geq 5$ deg we report a 4 sigma detection of large scale ($3\leq \ell \leq 8$) temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 76\pm 21 \mu\rm{K_{RJ}}^2$ and set upper limits to the $E$ and $B$ modes at $11 \mu\rm{K_{RJ}}^2$. For Galactic latitudes $|b| \geq 10$ deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 24\pm 13 \mu\rm{K_{RJ}}^2$. These results are then extrapolated to 100 GHz to estimate the contamination in CMB measurements by polarized diffuse Galactic dust emission. The $TE$ signal is then $1.7\pm0.5$ and $0.5\pm0.3 \mu\rm{K^2_{CMB}}$ for $|b| \geq 5$ and 10 deg. respectively. The upper limit on $E$ and $B$ becomes $0.2 \mu\rm{K^2_{CMB}} (2\sigma)$. If polarized dust emission at higher Galactic latitude cuts is similar to the one we report here, then dust polarized radiation will be a major foreground for determining the polarization power spectra of the CMB at high frequencies above 100 GHz.

### Dates and versions

in2p3-00023663 , version 1 (12-12-2006)

### Identifiers

• HAL Id : in2p3-00023663 , version 1
• ARXIV :
• DOI :

### Cite

N. Ponthieu, J.F. Macias-Perez, M. Tristram, P. Ade, A. Amblard, et al.. Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops. Astronomy and Astrophysics - A&A, 2005, 444, pp.327-336. ⟨10.1051/0004-6361:20052715⟩. ⟨in2p3-00023663⟩

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