\begin{table}%t2
%\centering
\par
\caption{\label{tab:comb_em}Worksheet for estimating the magnitude of polconversion due to  bandpass mismatch in the \Planck\ frequency bands, over the full sky  (``4$\pi$'') and over pixels outside the \WMAP\ KQ85 mask (``Mask'').}
\begin{tabular}{ccccrrrrcrrr}
\hline \hline\noalign{\smallskip}
& & \multicolumn{2}{c}{CMB emission} & 
\multicolumn{4}{c}{Foreground emission} & & & 
\multicolumn{2}{c}{Polconversion ${\cal M}_{QI}I^{\rm F}$} \\ 
Band & Region & $\sigma(I)$\tablefootmark{a} & $\sigma(Q,U)$\tablefootmark{a} & $\langle I^{\rm F} \rangle$\tablefootmark{b} &  $\langle \sqrt{Q^2+U^2}\rangle$\tablefootmark{c} &
$\langle \beta \rangle$\tablefootmark{b} & $\tilde{\beta}$\tablefootmark{b,d} & $\nu_0$ & $\sigma(\nu_{\rm eff})$\tablefootmark{e} & rms\tablefootmark{f} &  Abs Max\tablefootmark{f} \\
& & ($\mu$K) & ($\mu$K) & ($\mu$K) & ($\mu$K) & & & (GHz) & (GHz) &  ($\mu$K) &  ($\mu$K) \\
\hline
\multirow{2}{*}{30~GHz} & $4\pi$ & \multirow{2}{*}{85} & 
\multirow{2}{*}{0.94}
& 410 & 13 & $-$2.89 & $-$2.63 & \multirow{2}{*}{28.11} & \multirow{2}{*}{0.29} & 28.0 & 1300 \\
       & Mask   &      &     & 110 & 10 & $-$2.92 & $-$2.87 &  & &
    1.7 & 28 \\
\multirow{2}{*}{44~GHz} & $4\pi$ & \multirow{2}{*}{89} & 
\multirow{2}{*}{1.31}
 & 130 & 4 & $-$2.61 & $-$2.36 & \multirow{2}{*}{43.81} & \multirow{2}{*}{0.21}
  & 4.6 & 210 \\
       & Mask   &      &     &  30 & 3 & $-$2.64 & $-$2.56 & & &
    0.2 & 2 \\
\multirow{2}{*}{70~GHz} & $4\pi$ & \multirow{2}{*}{89} & 
\multirow{2}{*}{1.91}
 &  60 & 3 & $-$0.46 & $-$0.60 & \multirow{2}{*}{69.54} & \multirow{2}{*}{1.35}
 & 1.9 & 140 \\
       & Mask   &      &     &  16 &  2 & $-$0.46 & $-$0.24 & & &
    0.1 & 12 \\
\hline 
\end{tabular}
\tablefoot{$\langle X \rangle$ denotes area-weighted mean values.
\citet{PLP_R3} bandpasses were used to calculate $\nu_0$, $\nu_{\rm eff}$, and ${\cal M}_{QI}$. \tablefoottext{a}{rms after convolution with the beam;}
\tablefoottext{b}{foreground temperature, $I^{\rm F}$, and spectral index, $\beta$, from the \Planck\ sky model;}
\tablefoottext{c}{foreground polarisation, interpolated from \WMAP;}
\tablefoottext{d}{flux-weighted mean spectral index;}
\tablefoottext{e}{standard deviation of $\nu_{\rm eff}(\bar{\beta})$ over the  detectors in each band;}
\tablefoottext{f}{rms and extreme value of the polconversion signal 
(mean over RCAs in each band).}}\vspace*{2.5mm}
\end{table}