\begin{table}%t1
\caption{Models of the nova spatial distribution in the Galaxy used for the Monte~Carlo simulations \citep{Jean2000}. }
\label{table_Jean2000}
\small%\centerline
 {
\begin{tabular}{lll}
\hline \hline
\multicolumn{3}{l}{{Model 1} \citep{KDF91}:} \\
\multicolumn{3}{l}{$\rho_{\rm h}$ = 3.0 kpc and $z_{\rm h}$ = 0.170 kpc. $K_{0}$ is the modified Bessel function} \\
\hline  
\multicolumn{1}{l}{Disc $n(z,\rho)$} &  = $n_{\rm d} \exp \Big( -\frac{|z|}{z_{\rm h}} - \frac{\rho}{\rho_{\rm h}} \Big)$   & \\ 
\multicolumn{1}{l}{Bulge $n(R)$}  &   = $n_{\rm s} 1.04 \times 10^{6} \Big( \frac{R}{0.482} \Big)^{-1.85}$  &  $R \leq 0.938$ kpc \\ 
                 & = $n_{\rm s} 3.53 K_{0} \Big( \frac{R}{0.667} \Big)$  &  $R \geq 0.938$ \\[6pt]
                 & $= 0$  &  $R \geq 5$ kpc \\ 
\hline  
\multicolumn{3}{l}{{Model 2} \citep{VdK90}:} \\
\multicolumn{3}{l}{$\rho_{\rm h}$ = 5.0 kpc and $z_{\rm h}$ = 0.30 kpc} \\
\hline  
&& \\[-8pt]
\multicolumn{1}{l}{Disc $n(z,\rho)$} & = $n_{\rm d} \exp \Big( -\frac{|z|}{z_{\rm h}} - \frac{\rho}{\rho_{\rm h}} \Big)$   & \\ 
\multicolumn{1}{l}{Bulge $n(R)$} &    = $n_{\rm s} 1.25 \Big( \frac{R}{R_{\rm g}} \Big)^{-6/8} \exp \Big[ -10.093 \Big( \frac{R}{R_{\rm g}} \Big)^{1/4} + 10.093 \Big]$  &  $R \leq R_{\rm g}$ \\ 
                 & $= n_{\rm s} \Big( \frac{R}{R_{\rm g}} \Big)^{-7/8} \Bigg[ 1-\frac{0.0867}{ \big( \frac{R}{R_{\rm g}} \big)^{1/4}} \Bigg] \exp \Big[ -10.093 \Big( \frac{R}{R_{\rm g}} \Big)^{1/4} + 10.093 \Big]$  &  $R \geq R_{\rm g}$ \\
&& \\[-8pt]                  
\hline  
\multicolumn{3}{l}{{Model 3} \citep{DJ94}:} \\
\multicolumn{3}{l}{$\rho_{\rm h}$ = 5.0 kpc and $z_{\rm h}$ = 0.35 kpc} \\
\hline  
&& \\[-8pt]
\multicolumn{1}{l}{Disc $n(z,\rho)$}& = $n_{\rm d} \exp \Big( -\frac{|z|}{z_{\rm h}} - \frac{\rho}{\rho_{\rm h}} \Big)$   & \\ 
\multicolumn{1}{l}{Bulge $n(R)$}&  = $\frac{n_{\rm s}}{R^{3}+0.343}$ &  $R \leq 3$ kpc \\[1mm] 
& $= 0$  &  $R \geq 3$ kpc \\ 
\hline 
\end{tabular}}
\medskip
$R$ is the distance from the Galactic Centre, $z$ is the distance perpendicular to the Galactic plane and $\rho$ is the galactocentric planar distance. The distance from the Galactic Centre to the Sun is $R_{\rm g} = 8$~kpc, $n_{\rm s}$ and $n_{\rm d}$ are the normalisation factors for the bulge and the disc respectively (in kpc$^{-3}$). The proportions of novae in the bulge are 0.179 (Model~1), 0.105 (Model~2) and 0.111 (Model~3).
\end{table}