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We present the first measurement of temperature and polarization angularpower spectra of the diffuse emission of Galactic dust at 353 GHz as seen byArcheops on 20% of the sky. The temperature angular power spectrum iscompatible with that provided by the extrapolation to 353 GHz of IRAS and DIRBEmaps using \cite{fds} model number 8. For Galactic latitudes $|b| \geq 5$ degwe 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 sameangular scales, we report a 2 sigma detection of temperature-polarizationcross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 24\pm 13 \mu\rm{K_{RJ}}^2$. Theseresults are then extrapolated to 100 GHz to estimate the contamination in CMBmeasurements by polarized diffuse Galactic dust emission. The $TE$ signal isthen $1.7\pm0.5$ 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 issimilar to the one we report here, then dust polarized radiation will be amajor foreground for determining the polarization power spectra of the CMB athigh frequencies above 100 GHz.Comment: 11 pages, 8 figures, submitted to A

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