\begin{table}%T1
  \caption{\label{tab:locations}Numerical summary$^\dagger ~ ^\ddagger$ for the VHE and $E>100$~MeV sources in the W~28 region including 
    positional and spectral information.}
  \small%\centerline
{
  \begin{tabular}{llllllll}
  \hline \hline
    & \multicolumn{2}{c}{Best fit position (J2000.0)} & & & \multicolumn{2}{c}{Spectral analysis} & \\ \cline{2-3} \cline{6-7} \\[-2mm]
   Name & RA [deg] & Dec [deg] & $^1$$\sigma_{\rm src}$ [deg] & $^2$$S$ [$\sigma$] (evts) & $^3 k$ & $^4 \Gamma$ & $^5 L$\\ \hline 
   HESS~J1801$-$233  & 270.426 $\pm$ 0.031 & $-$23.335 $\pm$ 0.032 & 0.17 $\pm$ 0.03 & +7.9 (281) & 7.50 $\pm$ 1.11 $\pm$ 0.30 & 2.66 $\pm$ 0.27 & 1.5\\
   HESS~J1800$-$240A$^\S$ & 270.491 $\pm$ 0.001 & $-$23.962 $\pm$ 0.001 & 0.15     & +6.0 (180) & 7.65 $\pm$ 1.01 $\pm$ 0.50 & 2.55 $\pm$ 0.18 & 1.5 \\ 
   HESS~J1800$-$240B$^\S$ & 270.110 $\pm$ 0.002 & $-$24.039 $\pm$ 0.009 & 0.15     & +7.8 (236) & 7.58 $\pm$ 0.90 $\pm$ 0.15 & 2.50 $\pm$ 0.17 & 1.4 \\
   HESS~J1800$-$240C & 269.715 $\pm$ 0.014 & $-$24.052 $\pm$ 0.006 & 0.02 $\pm$ 0.15 & +4.5 (71) & 4.59 $\pm$ 0.89 $\pm$ 0.20 & 2.31 $\pm$ 0.35 & 0.8 \\
   HESS~J1800$-$240$^{\S\S}$  & 270.156 $\pm$ 0.044 & $-$23.996 $\pm$ 0.022 & 0.32$^{\rm RA}$ $\pm$ 0.05& +10.3 (652) & 18.63 $\pm$ 1.85 $\pm$ 1.20 & 2.49 $\pm$ 0.14 & 3.6\\  
                                          &                     &                       & 0.17$^{\rm Dec}$ $\pm$ 0.03 & \\ 
   GRO~J1801$-$2320  & 270.360 $\pm$ 0.150 & $-$23.340 $\pm$ 0.150 &  --  & +13.2        & 3.35 $\pm$ 0.52 & 2.16 $\pm$ 0.10 & 480.0 \\ 
     \hline
     \end{tabular}  }
   \smallskip
    $\dagger$ VHE photon spectra are derived from a region of radius 
     $\theta = \sqrt{0.1^2+\sigma_{\rm src}^2}$ centered on each source's position unless otherwise indicated. \\
   $\ddagger$ In spectra, a function 
     ${\rm d}N/{\rm d}E = k E^{-\Gamma}$ ph~cm$^{-2}$~s$^{-1}$~TeV$^{-1}$ is fitted. $E$ is in TeV units (HESS data); GeV units (EGRET data). \\
    $1.$ Fitted intrinsic source size (Gaussian std. dev.).\\
  $2.$ Statistical significance and excess events in brackets; for HESS sources using Li \& Ma (\cite{Li:1}); for EGRET sources given by $S=\sqrt{T_{\rm s}}$ for $T_{\rm s}$~defined by Mattox \etal (\cite{Mattox:1}). \\
 $3.$ For HESS sources: $\times 10^{-13}$ ph cm$^{-2}$ s$^{-1}$~TeV$^{-1}$ at 1~TeV (with statistical and systematic errors); For EGRET sources:  $\times 10^{-2}$~ph~cm$^{-2}$~s$^{-1}$~GeV$^{-1}$ at~1~GeV (with statistical errors).\\
     $4.$ Only statistical errors indicated. Systematic error is estimated at $\pm$0.2.\\
  $5.$ Luminosity $\times 10^{33}$~erg~s$^{-1}$ at 2~kpc (0.3 to 3 TeV for HESS; 0.04 to 6~GeV for EGRET).\\
   $^\S$ Due to cross contamination between components A \& B, a fixed value of $\sigma_{\rm src}= 0.15^\circ$ estimated visually from Fig.~\ref{fig:tevskymap} was used. \\
   $^{\S\S}$ Spectrum extracted from a 0.8$^\circ \times 0.6^\circ$ elliptical region 
     encompassing all components A, B, C, and matching the size of the corresponding molecular cloud.  
\end{table}