\begin{table}%T1
\caption{Candidate stars associated with HII\ regions.}
\label{tab:uchii}
%\centerline
{
\begin{tabular}{lllcccccc}\hline\hline
Radio source & RA (2000) & Dec (2000) & $J$ & $H$ & $K$s & $J-H$ & $H-K{\rm s}$ & Inferred mass ($M_{\odot}$)\\\hline
CC & 19:10:11.60 & 9:07:06.5 & $19.09\pm0.02$  & $15.78\pm0.02$ & $13.92\pm0.04$ & 3.31 & 1.86 & 56 \\
F  & 19:10:13.42 & 9:06:22.0 & --    & $15.80\pm0.01$ & $11.94\pm0.02$ & --  & 3.86 & $>$120?\\
J2 & 19:10:14.22 & 9:06:27.4 & --    & $17.36\pm0.01$ & $15.45\pm0.02$ & --  & 1.91 & 25 \\
O3 & 19:10:16.92 & 9:06:10.9  & $18.61\pm0.02$  & $15.54\pm0.02$ & $13.90\pm0.03$ & 3.07 & 1.64 & 46  \\
RQ & 19:10:10.76 & 9:05:18.2  & --    & $19.18\pm0.03$ & $15.87\pm0.03$ & --  & 3.31 & 78   \\
RQ & 19:10:10.93 & 9:05:15.9  & --    & $17.33\pm0.02$ & $15.63\pm0.02$ & --  & 1.70 & 18   \\
RQ & 19:10:10.96 & 9:05:17.7  & --    & $18.57\pm0.03$ & $12.94\pm0.02$ & --  & 5.64 & $>$120? \\
RQ & 19:10:11.16 & 9:05:11.6  & $17.84\pm0.01$  & $15.51\pm0.02$ & $14.36\pm0.02$ & 2.34 & 1.14 & 21 \\
S  & 19:10:11.66 & 9:05:27.5  & $16.48\pm0.02$  & $14.16\pm0.02$ & $13.02\pm0.04$ & 2.32 & 1.14 & 46 \\
S  & 19:10:11.80 & 9:05:27.1 & --     & $18.19\pm0.04$ & $15.23\pm0.05$ & --  & 2.96 & 80 \\
S  & 19:10:11.83 & 9:05:28.3 & --     & $17.21\pm0.03$ & $14.57\pm0.04$ & --  & 2.64 & 84 \\
S  & 19:10:11.88 & 9:05:28.2 & --     & $16.73\pm0.01$ & $14.40\pm0.02$ & --  & 2.33 & 68 \\
South & 19:10:21.90 & 9:04:57.1 & -- & $17.60\pm0.02$ & $14.96\pm0.04$ & --  & 2.64 &  68 \\
South & 19:10:22.08 & 9:05:00.0 & -- & $17.43\pm0.02$ & $14.54\pm0.03$ & --  & 2.89 &  111 \\
South & 19:10:22.09 & 9:05:01.5 & -- & $19.02\pm0.04$ & $16.29\pm0.02$ & --  & 2.73 &  36 \\
South & 19:10:21.97 & 9:05:04.2 & -- & $16.61\pm0.02$ & $14.54\pm0.03$ & --  & 2.07 &  49 \\
South & 19:10:22.20 & 9:05:04.2 & -- & $18.23\pm0.03$ & $16.19\pm0.02$ & --  & 2.05 &  19   \\
South & 19:10:21.90 & 9:04:58.1 & -- & $16.78\pm0.05$ & $14.74\pm0.04$ & --  & 2.04 &  42 \\
South & 19:10:22.20 & 9:05:01.5 & -- & $18.06\pm0.03$ & $15.84\pm0.04$ & --  & 2.22 &  28 \\
South & 19:10:21.80 & 9:05:03.3 & -- & $18.33\pm0.03$ & $14.34\pm0.05$ & --  & 3.99 & $>$120? \\
South & 19:10:21.88 & 9:05:04.3 & $20.07\pm0.04$ & $15.36\pm0.01$ & $12.74\pm0.03$ & 4.71 & 2.62 & $>$120? \\
South & 19:10:21.75 & 9:05:04.3 & -- & $18.61\pm0.03$ & $14.88\pm0.05$ & --  & 3.73 & $>$120?\\
South & 19:10:22.24 & 9:05:00.3 & -- & $18.46\pm0.01$ & $16.29\pm0.03$ & --  & 2.17 & 20  \\
South & 19:10:22.02 & 9:05:00.3 & -- & $18.27\pm0.03$ & $16.11\pm0.05$ & --  & 2.16 & 22  \\
South & 19:10:22.00 & 9:05:06.5 & -- & $18.56\pm0.03$ & $16.36\pm0.04$ & --  & 2.20 & 20  \\\hline
\end{tabular}}
\par
\medskip
Notes: names are from De~Pree et~al. (1997).
Sources associated with RQ, S, and W49 South are likely 
to be multiple unresolved objects; nebular emission near these sources 
complicates the determination of the background and likely makes the errors in the photometry
larger than the quoted formal photometric errors. Masses are inferred from the 
extinction-corrected $K$~magnitudes, a distance of 11.4~kpc, and $4\times10^{5}$~yr
stellar tracks from Lejeune \& Schaerer (2002) with solar metallicity and
enhanced mass loss. Objects with only $H$ \& $K$s~magnitudes may have an unknown 
$K$s excess which could severely affect the inferred mass. Five objects 
have inferred masses above $120 ~M_{\odot}$, which is likely due to a $K$s~excess
and/or multiplicity. Errors of $10{-}20$\% in the mass estimate are expected simply
from the uncertainty in the distance.
\end{table}