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

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 $\mathrm{\mid }b\mathrm{\mid }\ge 5$ deg we report a 4 sigma detection of large scale ($3\le \mathrm{\ell }\le 8$) temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 76\pm 21 \mu\rm{K_{RJ}}^2$andsetupperlimitstothe$E$and$B$modesat$11 \mu\rm{K_{RJ}}^2$\mathrm{.}ForGalacticlatitudes$|b| \geq 10$ deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation $(\mathrm{\ell }+1)C_{\mathrm{\ell }}^{TE}\mathrm{/}2\pi =24\pm 13\mu {{\mathrm{K}}_{\mathrm{R}\mathrm{J}}}^2$. 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 $1.7\pm 0.5$ and $0.5\pm 0.3\mu {\mathrm{K}}_{\mathrm{C}\mathrm{M}\mathrm{B}}^2$ for $\mathrm{\mid }b\mathrm{\mid }\ge 5$ 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.