\begin{table}%t10
\caption{\label{LTIR}Luminosities, size and SFR of our galaxies.}
\small%\centerline
 {
 \begin{tabular}{cc|ccc}
\hline
\hline
&&&& \\[-8pt]
\multicolumn{2}{c|}{}   & NGC~1705 $^a$& Haro~11 $^a$  & Mrk~1089 \\
\hline
&&&& \\[-8pt]
\multicolumn{1}{c}{$L_{\rm TIR}$ = $L_{[3~\mu {\rm m},1100~\mu {\rm m}]}$ (\lsun)} $^b$ &  {\small (1)}   &  5.8 $\times$ 10$^7$ &  1.7 $\times$ 10$^{11}$   & 3.9 $\times$ 10$^{10}$ \\ 
& {\small (2)}    & 4.9 $\times$ 10$^7$& 1.4 $\times$ 10$^{11}$  &   3.8 $\times$ 10$^{10}$\\
& {\small (3)}   & 5.9 $\times$ 10$^7$&  1.6 $\times$ 10$^{11}$   &    4.3 $\times$ 10$^{10}$ \\
$L_{[3~\mu{\rm m},50~\mu{\rm m}]}$ (\lsun) 	&   &   1.9 $\times$ 10$^{7}$	&  1.2 $\times$ 10$^{11}$   &  1.4 $\times$ 10$^{10}$\\
$L_{[50~\mu{\rm m},100~\mu{\rm m}]}$ (\lsun) &	 & 2.2 $\times$ 10$^{7}$& 4.1 $\times$ 10$^{10}$    & 1.3 $\times$ 10$^{10}$  \\
$L_{[100~\mu{\rm m},1100~\mu{\rm m}]}$ (\lsun) 	&  & 1.6 $\times$ 10$^{7}$&  9.6 $\times$ 10$^{9}$    & 1.1 $\times$ 10$^{10}$ \\
$L_{\rm FIR}$  = $L_{[8~\mu{\rm m},1100~\mu{\rm m}]}$ (\lsun) &  & 5.1 $\times$ 10$^{7}$&  1.6 $\times$ 10$^{11}$   & 3.7 $\times$ 10$^{10}$  \\
$L_{\rm H\alpha}$ (erg s$^{-1}$) $^c$ 	&   &   6.34 $\times$ 10$^{38}$ &  3.2 $\times$ 10$^{42}$    &  4.57 $\times$ 10$^{41}$ \\
Size &&  0.5$'$ $\times$ 0.5$'$ & 0.25$'$ $\times$ 0.25$'$ & 0.31$'$ $\times$ 0.12$'$ \\
SFR (\msun\  yr$^{-1}$  kpc$^{-2}$) $^d$& (4)    & 1.6 $\times$ 10$^{-3}$ &5.1 $\times$ 10$^{-2}$  & 5 $\times$ 10$^{-2}$\\
 & (5)    & 9.4 $\times$ 10$^{-4}$& --  & 5.8 $\times$ 10$^{-2}$\\
 & (6)    & 5.2 $\times$ 10$^{-4}$& 2.4 $\times$ 10$^{-2}$  & 1.4 $\times$ 10$^{-2}$ \\
 & (7)    & 5.7 $\times$ 10$^{-4}$& 3 $\times$ 10$^{-2}$  & 1.8 $\times$ 10$^{-2}$\\
\hline
\end{tabular}}
\medskip
$^a$ The models used for NGC~1705 and Haro~11 include an independent, very cold dust component at 10~K with an emissivity $\beta$~=~1.  \\
$^b$ Total infrared luminosities ($L_{\rm TIR}$) are  estimated: 1)~by integrating our SED models with a submm constraint from 3 to 1100~\mic; 2)~from the \citet{Dale_Helou_2002} formula; 3)~from the \citet{Draine_Li_2007} formula. \\
$^c$~H$\alpha$ luminosities ($L_{\rm H\alpha}$) are given in \citet{Cannon_NGC1705_2006} for NGC~1705, \citet{Bergvall2000} for Haro~11 and c)~\citet{Iglesias-Paramo_Vilchez_1997} for Mrk~1089. \\ 
$^d$ Star formation rates (SFR) are estimated: 4)~using the relation of \citet{Kennicutt1998} based on $L_{\rm FIR}$; 5)~using the relation of \citet{Zhu2008} based on $\nu$~$L_{\nu}$[24~$\mu$m]. (this last relation is only valid for galaxies with a $L_{\rm TIR}$~$<$ 10$^{11}~L_{\odot}$  and can not be used for Haro~11); 6)~using the relation of \citet{Calzetti2007} based on the 24~\mic\ luminosity~($L_{24}$) alone; 7)~using the relation of \citet{Calzetti2007} based on~$L_{24}$ and~$L_{\rm H\alpha}$.
\end{table}