\begin{table}%t1
\caption{\label{table:polaris}SPIRE observations of the Polaris flare.}
\par
%\centerline
{\small
\begin{tabular}{cccccccc}
\hline\hline
$\lambda$ & Pixel size & {\it FWHM} & $G$ & $S_0$ & Noise & $\gamma$ & $P_{0}$ \\
($\mu$m) & (arcsec) & (arcsec) & & (MJy sr$^{-1}$) & (MJy sr$^{-1}$) & & (Jy$^2$ sr$^{-1}$) \\ \hline 
&&&&&&& \\[-3mm]
250 & 6 & 18.1 & $3.3\pm0.5$ (0.01) & $20.1\pm3.1$ (0.1) & 1.26 & $-2.65\pm0.10$ & $5\pm 2\times 10^3$\\
350 & 10 & 25.2 & $1.7\pm0.3$ (0.008) & $10.1\pm1.6$ (0.05) & 0.55 & $-2.69\pm 0.13$ & 4$\pm 2 \times 10^3$\\
500 & 14 & 36.9 & $0.7\pm0.1$ (0.003) & $4.3\pm0.7$ (0.02) & 0.34 & $-2.62\pm 0.17$ & $1\pm 1 \times 10^3$\\ \hline
\end{tabular}}
\tablefoot{Columns~4 and~5: gain and offset coefficients of the SPIRE-IRIS~100~$\mu$m correlations. 
The uncertainty on $G$ represents the rms of the ratio $S(\lambda)/S(100~\mu{\rm m})$ once the offset $S_0$ is removed from the SPIRE data. Similarly the uncertainty on $S_0$ is the rms of $S(\lambda) - G\times S(100~\mu{\rm m})$. These two uncertainties are correlated, but they give more realistic estimates compared to the statistical ones obtained with the linear regression fit (given in brackets). Column~6: noise level estimated directly on the power spectrum for $k>0.75k_{\rm max}$ ($3.75<k<5$~arcmin$^{-1}$ at 250~$\mu$m). Column~7: power spectrum exponent of the interstellar component. Column~8: level of the Poissonian component associated with point sources and the CIB fluctuations. The fit of the power spectrum ($\gamma$ and $P_0$) was done between $k=0.025$~arcmin$^{-1}$ and about twice the {\it FWHM} (2.0, 1.2 and 0.86~arcmin$^{-1}$ at 250, 350 and 500~$\mu$m respectively).}\vspace*{3mm}
\vspace{-5mm}\end{table}