\begin{table}
\caption{Summary of \textit{Planck} instrument performance in flight, as predicted from ground
characterisation (Mennella et al. \cite{LFICal}; Lamarre et al. \cite{HFIInst})}  \label{TabInstPar}
%\tableline
\renewcommand{\footnoterule}{}  % to avoid a line before footnotes
%\centering
\par
\begin{tabular}{l|ccc|cccccc}
\par
 \hline\hline 
 Instrument & \multicolumn{3}{|c|}{LFI} & \multicolumn{6}{|c}{HFI} \\
 \hline
Center frequency [GHz]&30&44&70&100&143&217&353&545&857\\
Number of polarised detectors\tablefootmark{a}%\footnote{For the LFI, the values shown correspond to the output of a
% linearly polarised differential radiometer; two such outputs, referred to as ``detectors" in this
% paper, are supported by each horn. In fact each of the two radiometer outputs from one horn is built
% from the data acquired by two diodes, each of which are switched at high frequency between the sky
% and a blackbody load at 4 K (see Bersanelli et al. \cite{LFIInst}). For the HFI, a (polarised) detector is taken to be
% the output of one of a pair of linearly polarised polarisation-sensitive bolometers; each horn
% contains one pair, i.e. two orthogonally-polarised detectors. Unpolarised spider-web bolometers are
% present in some of the horns, in these cases there is only one detector per horn. See
% Lamarre et al. (\cite{HFIInst}).}
 &4&6&12&8&8&8&8& & \\
Number of unpolarised detectors
 & & & & &4&4&4&4&4\\
Mean\tablefootmark{b}%\footnote{Band-averaged, including polarised and unpolarised detectors, see Tauber et al. (\cite{SystOpt}).} 
FWHM (arcmin)
& 32.7 & 29.5 & 13.0 & 9.6 & 7.0 & 4.6 & 4.5 & 4.7 & 4.3\\
Mean\tablefootmark{c}%\footnote{Band-averaged, including polarised and unpolarised detectors, see Tauber et al. (\cite{SystOpt}).}
 ellipticity
& 1.36 & 1.50 & 1.27 & 1.17 & 1.05 & 1.11 & 1.13 & 1.03 & 1.04\\
Bandwidth ($\Delta\nu$, GHz)& 4.5& 4.1& 12&32&45&68&104&174&258\\
%Lower band edge ($\nu$, GHz)& & & & & & & & & \\
%Upper band edge ($\nu$, GHz)& & & & & & & & & \\
${\Delta T/T}$ per pixel (Stokes $I$)\tablefootmark{d}%\footnote{In $\mu$K/K (thermodynamic temperature) for 15 months
% integration, $1\sigma$, for square pixels whose sides are given in the row ``Mean FWHM". The
% instantaneous sensitivities used for these estimates are drawn from ground calibration, averaged for
% all detectors in each channel; for LFI the sensitivity is the mean of the two methods described in
% Mennella et al. (\cite{LFICal}).}
 &3.3 &5.2 &8.9 & 3 &2.2 &4.8 &2.0  &150 &6000 \\
 ${\Delta T/T}$ per
pixel (Stokes $Q$ \&$U$)\tablefootmark{e}%\footnote{$\sqrt{2}\times{\Delta T/T}(I)$.}
&4.6 &7.4 &12.7 &4.8 &4.1 &9 &38 & & \\
Point source sensitivity\tablefootmark{f}%\footnote{Not including background confusion. Estimates of confusion levels can be extracted from Leach et al. (\cite {Leach2008}).}
 (1$\sigma$, mJy) & 22 &59 &46 & 14& 10& 14& 38& 44& 45 \\
%Estimated confusion level\footnote{Including CMB and other diffuse foregrounds, compact sources, instrument noise etc} (mJy) & & & & & & & & & \\
\hline
\end{tabular} 
\tablefoot{\tablefoottext{a}{For the LFI, the values shown correspond to the output of a
linearly polarised differential radiometer; two such outputs, referred to as ``detectors'' in this
paper, are supported by each horn. In fact each of the two radiometer outputs from one horn is built
from the data acquired by two diodes, each of which are switched at high frequency between the sky
and a blackbody load at 4 K (see Bersanelli et al. \cite{LFIInst}). For the HFI, a (polarised) detector is taken to be
the output of one of a pair of linearly polarised polarisation-sensitive bolometers; each horn
contains one pair, i.e. two orthogonally-polarised detectors. Unpolarised spider-web bolometers are
present in some of the horns, in these cases there is only one detector per horn. See
Lamarre et al. (\cite{HFIInst}).}\protect\newline \tablefoottext{b}{Band-averaged, including polarised and unpolarised detectors, see Tauber et al. (\cite{SystOpt}).}\protect\newline \tablefoottext{c}{Band-averaged, including polarised and unpolarised detectors, see Tauber et al. (\cite{SystOpt}).}\protect\newline
\tablefoottext{d}{In $\mu$K/K (thermodynamic temperature) for 15 months
integration, $1\sigma$, for square pixels whose sides are given in the row ``Mean FWHM''. The
instantaneous sensitivities used for these estimates are drawn from ground calibration, averaged for
all detectors in each channel; for LFI the sensitivity is the mean of the two methods described in
Mennella et al. (\cite{LFICal}).}\protect\newline \tablefoottext{e}{$\sqrt{2}\times{\Delta T/T}(I)$.}\protect\newline \tablefoottext{f}{Not including background confusion. Estimates of confusion levels can be extracted from Leach et al. (\cite {Leach2008}).}}
\end{table}