\begin{table}%t3
\caption{\label{tab:NH}Column density in units of $10^{22}~\rm cm^{-2}$ for the six observations and the sine fit, obtained with different continuum models.}
\par
%\centering
\small
\begin{tabular}{cccccccc}
\hline \hline\noalign{\smallskip}
Observation or fit	        & X2	             & S1	                  & S3	   & C1	           & S2	          & X1	                  & Sine fit \\
 $\phi_{\rm orb}^{\rm (T3)}$             & 0.17--0.28             & 0.37--0.42             & 0.43--0.50             & 0.45--0.51                & 0.49--0.61       & 0.94--0.96                & full orbit \\[2pt]
  \hline\noalign{\smallskip}
\texttt{diskbb~+~powerlaw}\tablefootmark{*} & $\left(2.00^{+0.17}_{-0.19}\right)$\tablefootmark{*} & $\left(1.2^{+0.5}_{-0.2}\right)$\tablefootmark{*}    & $\rm 0.96^{+0.03}_{-0.02}$ & $\left(1.25^{+0.04}_{-0.01}\right)$\tablefootmark{*}    & $1.031\pm0.017$  & $\left(1.81^{+0.06}_{-0.05}\right)$\tablefootmark{*}    & $\left(1.43\pm0.43\right)$\tablefootmark{*} \\
\texttt{eqpair}                  & $1.279\pm0.005$        & $\rm 1.17^{+0.15}_{-0.10}$ & $1.02\pm0.02$          & $\rm 1.065^{+0.000}_{-0.019}$ & $1.088\pm0.017$  & $\rm 1.191^{+0.006}_{-0.007}$ & $1.15\pm0.15$ \\
\texttt{simpl(kerrbb)}           & $1.278\pm0.005$        & $\rm 1.17^{+0.11}_{-0.10}$ & $\rm 1.01^{+0.03}_{-0.02}$ & $\rm 1.085^{+0.018}_{-0.016}$ & $1.088\pm0.017$  & $\rm 1.187^{+0.014}_{-0.012}$ & $1.15\pm0.14$ \\
\texttt{simpl(diskbb)}           & $1.288\pm0.016$\tablefootmark{\dagger} & $\rm 1.14^{+0.15}_{-0.11}$ & $0.97\pm0.02$          & $\rm 1.009^{+0.018}_{-0.017}$ & $1.038\pm0.017$  & $\rm 1.133^{+0.005}_{-0.004}$ & $1.10\pm0.18$ \\[2pt]
\hline
\end{tabular}
\tablefoot{Quoted errors are statistical uncertainties at the 90\% confidence level for the observations, but semi-amplitudes for the sine fits. \\
\tablefoottext{*}{The \texttt{diskbb~+~powerlaw} model overestimates $N_{\rm H}$ more, the more the \texttt{powerlaw} contributes at low energies, see text.}\\
\tablefoottext{\dagger}{As the lack of data above 2~keV did not allow us to constrain the power law with the \texttt{simpl} model, we only used \texttt{diskbb}.}}
\end{table}