\begin{table}%t4
\caption{\label{tab:xtok}X-ray luminosities in the $0.3{-}0.7$~keV band of various X-ray emitting components in gas-poor galaxies.}
\par
%\centerline
{
\begin{tabular}{c c c c c c c}
\hline\hline\noalign{\smallskip} 
Name &  $L_{{\rm X,~unres}} $   & $ L_{{\rm X,~sss}} $ & $ L_{{\rm X,~gas}} $ & $ L_{X}/L_{K} $ & $ (L_{X}/L_{K})_{{\rm corr}} $  & Age \\
& (${\rm erg \ s^{-1}} $) & (${\rm erg \ s^{-1}}) $ & (${\rm erg \ s^{-1}} $) & (${\rm erg \ s}^{-1} \ L_{K,\odot}^{-1} $) & (${\rm erg \ s}^{-1} \ L_{K,\odot}^{-1} $) & (Gyr) \\ 
   &  (1) &  (2) & (3) & (4) & (5) &(6) \\ 
\hline 
M~31 bulge  &  $ 1.1  \times 10^{38} $ &  $ 3.5  \times 10^{37} $ & $ 7.9 \times 10^{37} $ & $ (1.8 \pm 0.2) \times 10^{27} $ & $ (2.2 \pm 0.2) \times 10^{27} $ &6--10$^a$ \\ 
M~32        &  $ 6.4  \times 10^{35} $ &  $ 9.0  \times 10^{35} $ & --                    & $ (1.8 \pm 0.2) \times 10^{27} $ & $ (2.4 \pm 0.2) \times 10^{27} $ &4--10$^b$ \\ 
M~105       &  $ 6.4  \times 10^{37} $ &  $ 1.9  \times 10^{37} $ & --                    & $ (2.0 \pm 0.2) \times 10^{27} $ & $ (2.0 \pm 0.2) \times 10^{27} $ &8--15$^c$ \\
NGC~3377    &  $ 6.7  \times 10^{37} $ &  $ 1.1  \times 10^{37} $ & --                    & $ (3.9 \pm 0.6) \times 10^{27} $ & $ (2.4 \pm 0.6) \times 10^{27} $ & 4.1$^d$ \\
NGC~3585    &  $ 6.2  \times 10^{38} $ &          --             & --                    & $ (4.1 \pm 0.3) \times 10^{27} $ & $ (2.6 \pm 0.3) \times 10^{27} $ & 3.1$^d$ \\
NGC~4278    &  $ 5.5  \times 10^{38} $ &  $ 3.4  \times 10^{37} $ & $ 4.1 \times 10^{38} $ & $ (3.2 \pm 0.2) \times 10^{27} $ & $ (3.2 \pm 0.2) \times 10^{27} $ &10.7$^d$ \\ 
Sagittarius&  $ 3.5  \times 10^{32} $ &  $ 7.3  \times 10^{32} $ & --                    & $ (1.2 \pm 0.4) \times 10^{27} $ & $ (1.7 \pm 0.4) \times 10^{27} $ &6.5--9.5$^e$\\ 
Milky Way  &                      -- &                      -- & --                    & $ (3.4 \pm 1.0) \times 10^{27} $ & --                              &--         \\ 
\hline \\
\end{tabular}}
\tablefoot{(1) Luminosity of unresolved X-ray emission.
 (2) Luminosity of resolved supersoft sources.
 (3) Luminosity of ionized gas.
 (4) Observed X-ray to $K$-band ratio.
 (5) X-ray to $K$-band ratio transformed to the same point source detection sensitivity of 
 $ 2 \times 10^{36} \ {\rm erg \ s^{-1}} $.
  The errors in Cols.~(4) and (5) correspond to statistical uncertainties in X-ray count rates. 
  (6) Age of the stellar population. References for ages: 
\tablefoottext{a}{\citet{olsen},} 
\tablefoottext{b}{\citet{coelho},} 
 \tablefoottext{c}{\citet{gregg},} 
 \tablefoottext{d}{\citet{terlevich},} 
  \tablefoottext{e}{\citet{bellazzini}.} }\vspace*{2mm}
\end{table}