\begin{table}%t3
\caption{\label{tab:fit}Results of spectral fits of unresolved emission.}
\par
%\centerline
{
\small\begin{tabular}{c c c c c c c c c}
\hline
\hline
\noalign{\smallskip}
Name & $kT_{\rm MKL}$ & $\Gamma$ & $L_{\rm MKL}$  & $ L_{\rm PL} $ & $ L_{\rm LMXB} $  & $ L_{\rm MKL}/L_{\rm PL}$ & $ L_{\rm MKL}/(L_{\rm PL}-L_{\rm LMXB})$ & $ \chi^2 $/d.o.f   \\
& (keV) &  & ($ {\rm erg \ s^{-1}} $) & ($ {\rm erg \ s^{-1}} $)  & ($ {\rm erg \ s^{-1}} $) & & &\\ 
& (1)   &(2)&            (3)             &      (4)                     &        (5)                 &(6)&(7)&(8) \\
\hline 
M~31 bulge  & $ 0.32 \pm 0.01 $ &  $ 1.82 \pm 0.04 $ & $ 1.8 \times 10^{38} $ & $ 2.5 \times 10^{38} $  &                   --  & $ 0.72 $ &  $ 0.72 $ & $  473/223 $   \\     
M~32        & $ 0.60 \pm 0.13 $ &  $ 1.65 \pm 0.15 $ & $ 1.1 \times 10^{36} $ & $ 5.3 \times 10^{36} $  &                   --  & $ 0.21 $ &  $ 0.21 $ & $   76/70  $   \\     
M~60        & $ 0.80 \pm 0.01 $ &  $ 1.70 \pm 0.11 $ & $ 6.2 \times 10^{40} $ & $ 1.5 \times 10^{40} $  & $ 2.0 \times 10^{39} $ & $ 4.13 $ &  $ 4.77 $ & $ 1015/100 $   \\     
M~84        & $ 0.65 \pm 0.01 $ &  $ 1.45 \pm 0.12 $ & $ 3.0 \times 10^{40} $ & $ 1.1 \times 10^{40} $  & $ 1.5 \times 10^{39} $ & $ 2.73 $ &  $ 3.16 $ & $  385/122 $   \\     
M~105       & $ 0.64 \pm 0.05 $ &  $ 2.26 \pm 0.19 $ & $ 4.7 \times 10^{37} $ & $ 1.8 \times 10^{38} $  & $ 3.8 \times 10^{37} $ & $ 0.26 $ &  $ 0.33 $ & $   74/73  $   \\     
NGC~1291    & $ 0.31 \pm 0.03 $ &  $ 2.64 \pm 0.23 $ & $ 6.3 \times 10^{38} $ & $ 9.9 \times 10^{38} $  & $ 3.2 \times 10^{38} $ & $ 0.64 $ &  $ 0.94 $ & $  83/67   $   \\     
NGC~3377    & $ 0.4           $ &  $ 2.15 \pm 0.47 $ & ${<} 1.8 \times 10^{37} $ & $ 3.0 \times 10^{38} $  & $ 3.3 \times 10^{38} $ & $ {<}0.06 $ &       -- & $   45/34  $   \\     
NGC~3585    & $ 0.4           $ &  $ 2.75 \pm 0.61 $ & ${<} 8.0 \times 10^{38} $ & $ 2.5 \times 10^{39} $  & $ 3.0 \times 10^{39} $ & $ {<}0.32 $ &       -- & $    46/39 $   \\     
NGC~4278    & $ 0.47 \pm 0.06 $ &  $ 2.34 \pm 0.31 $ & $ 5.1 \times 10^{38} $ & $ 1.1 \times 10^{39} $  & $ 1.1 \times 10^{38} $ & $ 0.46 $ &  $ 0.52 $ & $ 151/132  $   \\     
NGC~4365    & $ 0.49 \pm 0.04 $ &  $ 1.67 \pm 0.17 $ & $ 2.4 \times 10^{39} $ & $ 2.8 \times 10^{39} $  & $ 9.0 \times 10^{38} $ & $ 0.86 $ &  $ 1.26 $ & $  128/98  $   \\     
NGC~4636    & $ 0.59 \pm 0.01 $ &  $ 2.64 \pm 0.05 $ & $ 1.1 \times 10^{41} $ & $ 1.3 \times 10^{40} $  & $ 4.1 \times 10^{38} $ & $ 8.46  $ &  $ 8.74$ & $ 1122/199 $   \\     
NGC~4697    & $ 0.33 \pm 0.03 $ &  $ 2.54 \pm 0.54 $ & $ 7.3 \times 10^{38} $ & $ 4.7 \times 10^{38} $  & $ 2.1 \times 10^{38} $ & $ 1.55 $ &  $ 2.81 $ & $  78/66   $   \\     
NGC~5128    & $ 0.62 \pm 0.01 $ &  $ -0.76 \pm 0.01$ & $ 2.1 \times 10^{39} $ & $ 3.0 \times 10^{40} $  & $ 5.1 \times 10^{37} $ & $ 0.07 $ &  $ 0.07 $ & $ 3547/435 $   \\     
Sagittarius& $ 0.4           $ &  $ 2.44 \pm 0.51 $ & ${<} 1.2 \times 10^{33}$  & $ 2.5 \times 10^{33} $  &                    -- & $ {<} 0.48 $ &  $ {<} 0.48 $ & $  18{/}20   $   \\     
\hline \\
\end{tabular}}
\tablefoot{(1) Temperature of the thermal emission. 
(2) Photon index of the power-law.
(3), 
(4) Luminosities of the thermal and power-law components in the $0.5{-}8$~keV energy range.
 (5) The combined luminosity of unresolved low-mass \mbox{X-ray} binaries brighter than $10^{35} \ {\rm erg \ s^{-1}}$  (but fainter than the sensitivity limit for the given  galaxy)  estimated from the $K$-band luminosity of the studied region and the average LMXB \mbox{X-ray} luminosity function of \citet{gilfanov}.
(6) The observed luminosity ratio of the soft thermal component to the power-law.
(7) Same as (6) but corrected for contribution of unresolved LMXBs. For NGC~3377 and NGC~3585, the predicted LMXB luminosity exceeds the observed luminosity of the power-law component, presumably  because of  a scatter in $X{/}K$ ratios for LMXBs, therefore no LMXB-corrected luminosity ratio is computed. 
(8) Goodness of fit.}\vspace*{2mm}
\end{table}