\begin{table}%t2
\par
\caption {\label{tab:radiometry}Characteristics of stellar radio sources in the \object{Wd~1} cluster.}
%\centerline
 {\begin{tabular}{lcllllllllc}
\hline\hline
\noalign{\smallskip}
Source ID & Spectral & 8.6~GHz\tablefootmark{d} & 4.8~GHz  & 2.5~GHz  & 1.4~GHz &  Spec. Index &
\multicolumn{2}{c}{Radio pos.\tablefootmark{e}}&$\Delta$\tablefootmark{f}&Notes\\
\tablefootmark{a,}\tablefootmark{b}& Type\tablefootmark{c} & (mJy)&(mJy)&(mJy)&(mJy)&&$16^{\rm h}47^{\rm m}$ & 
$-45^{\circ}$&($\arcsec$)&\\
\hline
 4(H)  &           & $0.8\pm0.08$  & $0.6\pm0.1$ &      &              &$+0.49\pm0.31$ &1.445&50~37.66&0.37&\\
 4&\raisebox{1.5ex}[0pt]{F2 Ia$^+$}&  $2.2\pm0.2$r\tablefootmark{h}  & $2.8\pm0.3$r &\raisebox{1.5ex}[0pt]{$3.3\pm0.3$\tablefootmark{g}} &\raisebox{1.5ex}[0pt]{$3.8\pm0.4$} &$-0.23\pm0.07$&&&&1\\
 9(C)  &           & $24.9\pm2.5$ & $18.1\pm1.8$ & $9.5\pm0.9$ & $7.8\pm0.8$  &$+0.68\pm0.07$&4.136&50~31.41&&\\
 9&\raisebox{1.5ex}[0pt]{sgB[e]}& $30.5\pm3.0$r& $28.4\pm2.8$r&$21.0\pm2.1$r&$24.5\pm2.5$r&$+0.16\pm0.07$&&&&\\
12a    & A5 Ia$^+$ &  $2.9\pm0.3$r & $2.9\pm0.3$ &  $3.5\pm0.4$ & $3.0\pm0.4$ &$-0.06\pm0.08$&2.151&50~59.23&0.61&1\\
15     & O9.5-B0.5Ia     &  $0.6\pm0.06$  & $0.7\pm0.1$ &$<$$0.6$\tablefootmark{i}&$<$1.1      &$>$0.0&6.648&50~30.31&0.54& \\
17     & O9.5-B0.5Ia     &  $1.7\pm0.2$  & $1.6\pm0.2$ &$3.2\pm0.3$ & $2.9\pm0.4$   &$-0.42\pm0.11$&6.183&50~49.40&0.50&\\
WR B& WN7     &  $4.3\pm0.4$r  & $4.8\pm0.5$r&$4.4\pm0.4$ & $4.0\pm0.4$   &$+0.04\pm0.07$&5.345&51~\phantom{1}5.21 &0.21&2\\
20     & RSG       &  $3.8\pm0.4$r & $4.2\pm0.4$r&$4.1\pm0.4$& $4.8\pm0.4$    &$-0.11\pm0.07$&4.679&51~23.81&0.33&2\\
26(A)  & RSG       & $20.1\pm2.0$r & $21.9\pm2.2$r& $18.4\pm1.8$r& ?          &$+0.07\pm0.11$&5.370&50~36.57&0.33&2\\
31b(WR V)& WN8      & $ 0.4\pm0.06$  & $0.4\pm0.1$&$<$$0.6$&$<$1.1          &$\phantom{+}0.00\pm0.50$&3.821&50~39.22&0.45&\\
32     & F5 Ia$^+$ & $0.4\pm0.06$  &  $0.4\pm0.1$ &$<$$0.6$&$<$1.1        &$\phantom{+}0.00\pm0.50$&3.675&50~43.70&0.31&\\
44(WR L) & WN9     & $0.4\pm0.06$  &$<$0.3&$<$0.6&$<$1.1        &$>$0.5&4.210&51~\phantom{1}7.34 &0.23&\\
D09-R1   &           & $0.7\pm0.07$  & $0.8\pm0.1$ &      &              &$-0.23\pm0.27$&9.075&51~10.23&0.31&\\
D09-R1? &\raisebox{1.5ex}[0pt]{BSG}&$6.5\pm1.2$r&$6.2\pm1.2$r&\raisebox{1.5ex}[0pt]{$11.0\pm1.2$r}&\raisebox{1.5ex}[0pt]{$17.2\pm1.7$r} &$-0.61\pm0.11$&&&&1, 3 \\
72(WR A) & WN7   &  $0.5\pm0.06$  &  $0.5\pm0.1$ &$<$$0.6$&$<$$1.1$        &$\phantom{+}0.00\pm0.40$&8.332&50~45.58&0.00&\\
75     &  RSG      &  $0.3\pm0.06$  &$<$$0.3$&$<$$0.6$&$<$$1.1$        &$>$$0.0$&8.933&49~58.92&0.46&\\
237(B) &           &  $1.8\pm0.2$  &  $1.8\pm0.2$ &  $1.9\pm0.2$ &  $2.0\pm0.4$         &$-0.06\pm0.10$&3.117&52~18.99&0.28&\\
237    &\raisebox{1.5ex}[0pt]{RSG}&  $5.6\pm2.2$r&  $7.5\pm2.1$r& $10.6\pm3.0$r& $11.2\pm1.9$r&$-0.35\pm0.19$&&&&1, 3\\
239(WR F) &  WC9d  &  $0.3\pm0.06$  &$<$$0.3$&$<$$0.6$&$<$$1.1$        &$>$$0.0$&5.196&52~25.63&0.50&\\
243(G) & LBV       &  $1.5\pm0.2$  &$0.9\pm0.1$ &$<$$0.6$&$<$$1.1$        &$+0.87\pm0.30$&7.496&52~29.28&0.32&\\
265(I) & F5 Ia$^+$ &  $2.3\pm0.3$r &$ 2.1\pm0.2$ & $1.7\pm0.2$ &  $1.8\pm0.4$   &$+0.20\pm0.11$&6.268&49~24.19&0.30& \\
 5(WR S)& WN10-11 & $0.3\pm0.06$   &$<$0.3&$<$0.6&$<$1.1        &$>$0.0&2.877&50~19.76 &0.91&4\\
16a(L) & A2 Ia$^+$ &  $1.6\pm0.3$ & $2.0\pm0.2$ &$2.8\pm0.3$ & $3.0\pm0.4$   &$-0.33\pm0.09$&6.688&50~41.99&0.93&4\\
D09-R2   & BSG   &  $0.7\pm0.06$  & $0.8\pm0.1$ &$1.2\pm0.2$ & $1.6\pm0.4$   &$-0.43\pm0.11$&6.867&50~37.17&0.70&4\\
\hline
\end{tabular}}
\vspace*{-1.5mm}
\tablefoot{1) Extended component. 
2) These sources are embedded in extended emission which may influence the flux estimates.  
3) Not clear if the extended emission is related to the compact radio source or the underlying optical source. 
4) The radio emission is offset from the stellar position by more than $3\times$ the position uncertainty introduced by phase-transfer i.e. 0.6~arcsec. Hence, association of radio emission with the optical source is uncertain.}
\tablefoottext{a}{Source numbers from \cite{Westerlund:1987}.}
\tablefoottext{b}{Alternate names from C02, \cite{Borgman:1970}, \cite{Negueruela:2005}, and \cite{Crowther:2006}.}
\tablefoottext{c}{Spectral types from C02, C05, \cite{Negueruela:2005} and \cite{Crowther:2006}.} 
\tablefoottext{d}{Fluxes derived from visibility modelling, corrected for the primary beam of the ATCA.}
\tablefoottext{e}{J2000 positions of model components at 8.6~GHz, assuming reference source 1657-56 at \mbox{$\alpha = 17$:01:44.853}, $\delta$~=~--56:21:55.964. The uncertainty in absolute radio position is estimated to be $\pm$0.1~arcsec.} 
\tablefoottext{f}{Separation of the optical and radio positions.}
\tablefoottext{g}{ For sources with two components at higher frequencies, when there is only one model component determined this 
represents a total flux at this frequency.}
\tablefoottext{h}{The symbol ``r'' denotes components that appear resolved by the ATCA at that frequency.} 
\tablefoottext{i}{Quoted upper limits are~$3\sigma$.}
\vspace*{3mm}
\end{table}