\begin{table} %[!ht]%t3
%\centering
\par
\caption{\label{tab3}Determination of $A_{V}$, $R$ from common upper level 
PH lines, and $R$ derived from stellar photometry.}
\vspace*{-2mm}
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%
\par
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\par
\begin{tabular}{lcrclclcc} 
\hline
\hline\noalign{\smallskip}
   &    &\multicolumn{4}{l}{PH Emission Lines} 
&\multicolumn{2}{l}{Stellar Photometry} & \\
Object & Obs.\tablefootmark{a} & PH~Pairs\tablefootmark{b} & $A_{V}$(mag) 
& $R$\tablefootmark{c} & $A_{V}$(H$\alpha$--H$\beta$)\tablefootmark{d} & Star/Cluster 
& $R$ & Ref. \\
\hline
M~8    & TP &  7~[6--12] & 2.10 & 4.35 &      & Herschel~36 
& 4.6--5.6, 5.3  & 2, 3 \\
        & G-R  & 11~[7--20] & 2.20 & 6.1~(5.0)\tablefootmark{e} & 2.1(1.4) 
& NGC~6523 & 4.6 & 4 \\
 M~16   & G-R  &  9~[7--18] & 2.80 & 5.2~(3.1,4.8)\tablefootmark{f}
& 3.2(2.3) & NGC~6611 & 4.8 & 5 \\
 M~17   & TP &  7~[6--12] & 3.50 & 4.1 & 2.35(2.0) & NGC~6618 
& 4.2 & 1 \\
        & G-R  &  9~[7--18] & 3.05 & 4.3~(3.1) & 3.4(2.7) 
& Star~1~(Fig.~\ref{fig1}, \ref{fig5}) & 4.5 $\pm$ 0.25 & TP   \\
 M~20   & G-R  & 14~[7--22] & 1.05 & 5.5~(3.1) & 0.8(0.8) 
& HD~164492 & 5.1 & 6, 7 \\
        &      &        &      &       &      & HD~164492 & 3.1 & 8 \\
 M~42     & E &  9~[7--19] & 2.15 & 5.8  & 2.2(1.5) 
& $\theta$$^{1}$ Ori~C & 5.5 & 9 \\
 NGC~3603 & G-R  &  8~[9--18] & 6.9 & 5.4~(3.1) & 7.4(5.5) 
& NGC~3603  &  4.3         & 10 \\
S~311    & G-R  & 10~[7--18] & 1.90 & 5.5~(3.1) & 2.1(1.5) & 
[NGC~2467 & 1.8--3.9] & 11 \\ 
 NGC~7027 & Z-R & 16~[6--22] & 3.9 & 4.4~(3.1)\tablefootmark{g} 
& 4.0~(3.1) & &  & \\
\hline
\end{tabular}
\vspace*{-1.5mm}
\tablefoot{
 \tablefoottext{a}{Observer, TP: this paper, G-R: Garcia-Rojas et~al. (\cite{Garcia2005}, \cite{Garcia2006}),
E: Esteban et~al. (\cite{Esteban2004}), Z-R: Zhang et~al. (\cite{Zhang2005}) and Rudy et~al. (\cite{Rudy1992}).}
 \tablefoottext{b}{Number of line pairs, in brackets the range of quantum numbers 
considered.}
\tablefoottext{c}{Determined from relation (2); values in brackets
used by G-R.} 
\tablefoottext{d}{From H$\alpha$--H$\beta$ ratio and $R$ of Col.~5; in brackets for
 $R = 3.1$.}
\tablefoottext{e}{For 4100~\AA\ $<$ $\lambda$, for shorter $\lambda$ see 
Garcia-Rojas et~al. (\cite{Garcia2007}).}
\tablefoottext{f}{$R = 3.1$ for 5500~\AA\ $<$ $\lambda$, $R = 4.8$ for $\lambda$ $<$
5500~\AA.} 
 \tablefoottext{g}{Value usually taken.}}
 \vspace*{-3mm}
  \tablebib{1: Chini et~al. (\cite{Chini1980}), Chini $\&$ Kr\"ugel (\cite{Chini1983}), Hoffmeister et~al.
(\cite{Hoffmeister2008}); 2: Hecht et~al. (\cite{Hecht1982}): 4.6--5.6; 
  3: Cardelli et~al. (\cite{Cardelli1989}): 5.0; 4: McCall et~al. (\cite{McCall1990}); 5: Chini et~al.
(\cite{Chini1980}), Chini $\&$ Wargau (\cite{Chini1990}), Chini et~al. (\cite{Chini1992});
 6: Anderson (\cite{Anderson1970}); 7: Lynds et~al. (\cite{Lynds1985}); 8: Kohoutek et~al. (\cite{Kohoutek1999});
9: Cardelli $\&$ Clayton (\cite{Cardelli1988}); 
  10: Pandey et~al. (\cite{Pandey2000});
11: Grubissich (\cite{Grubissich1969}), NGC~2467 may not be a physical cluster.}
 \end{table}