\begin{table}%t1
\par
\caption{\label{tab:obs}\label{tab1}Physical parameters for well observed massive-star forming regions in the Galaxy and in the LMC.}
\small%\centering
\par
\begin{tabular}{l|llll|lll|llll}
\hline\hline
&&&&&&&&&&&\\[-3mm]%\noalign{\smallskip}
 & &\multicolumn{3}{c|}{Cluster} && \multicolumn{2}{c|}{Superbubble} & \multicolumn{4}{c}{$\theta_{\star}$\tablefootmark{d}} \\%\cline{3-5}\cline{7-8}
 % \hline 
Name & $N_{\star}$\tablefootmark{a} & Age  & Distance  & Size\tablefootmark{b} & & Size\tablefootmark{b} 
 & Density\tablefootmark{c} & $B=1~\mu\rm{G}$ & $B=1~\mu\rm{G}$  & $B=10~\mu\rm{G}$  & $B=10~\mu\rm{G}$ \\
&&(Myr)&(kpc)&(pc)&&(pc)&($\rm cm^{-3}$) & $q=5/3$&$q=3/2$&$q=5/3$&$q=3/2$ \\
 \hline
 &&&&&&&&&&&\\[-3mm]%\noalign{\smallskip}
Cygnus OB1/3 & 38$^{(16)}$          & 2$-$6$^{(12)}$  & 1.8$^{(19)}$       & 24  &             
      & 80$-$100$^{(14)}$   & $0.01?$                 
	& $5\times 10^4$   & $4\times 10^2$  & $4\times 10^{0}$   & $2\times 10^{-2}$  \\ 
&&&&&&&&	$5\times 10^5$&$3\times 10^3$&$4\times 10^{1}$&$1\times 10^{-1}$\\ 
Cygnus OB2    & 750$^{(5)}$          & 3--4$^{(12)}$  & 1.4--1.7$^{(10)}$ & 60$^{(11)}$   &   & 450?$^{(5)}$        & 0.02$^{(5)}$          
	& $2\times 10^4$  & $9\times 10^1$ & $1\times 10^0$  & $4\times 10^{-3}$ \\
	&&&&&&&& $2\times 10^5$& $7\times 10^2$& $2\times 10^1$& $3\times 10^{-2}$\\ 
Orion OB1       & 30--100$^{(3)}$     & 12$^{(2)}$     & 0.45$^{(2)}$       & 10$^{(2)}$   &      & $140\times 300$$^{(3)}$  & 0.02--0.03$^{(4)}$  
	& $3\times 10^3$ & $4\times 10^1$ & $3\times 10^{-1}$  & $1\times 10^{-3}$ \\
&&&&&&&&	 $2\times 10^6$ & $7\times 10^3$& $2\times 10^2$& $3\times 10^{-1}$\\ 
Carina nebula  & ?                          & 3$^{(23)}$      & 2.3$^{(8)}$         & 20&                     & 110$^{(23)}$        & $0.01?$                
	& $2\times 10^4$  & $1\times 10^2$ & $1\times 10^0$  & $5\times 10^{-3}$ \\
&&&&&&&& $2\times 10^6$& $7\times 10^3$&	 $1\times 10^2$& $3\times 10^{-1}$\\ 
Westerlund 1   & 450$^{(1)}$          & 3.3$^{(1)}$    & 3.9$^{(13)}$        &1$^{(1)}$&           & 40?$^{(13)}$       & $0.01?$                
	& $2\times 10^3$  & $5\times 10^1$ & $2\times 10^{-1}$ & $2\times 10^{-3}$ \\  &&&&&&&  $3\times 10^6$& $2\times 10^4$& $3\times 10^2$ & $8\times 10^{-1}$\\
Westerlund 2   &14$^{(21)}$           & 2$^{(21)}$     & 8$^{(21)}$           &1$^{(6)}$ &          & 100$^{(21,6)}$     & 0.0015$^{(24)}$   
	& $1\times 10^2$  & $2\times 10^0$ & $9\times 10^{-3}$ & $1\times 10^{-4}$ \\ 
		&&&&&&&&   $5\times 10^4$& $2\times 10^2$&
	 $4\times 10^0$&  $1\times 10^{-2}$\\
DEM L192       & 135                        & 3$^{(20)}$    & 50                       & 60$^{(20)}$&       & $120 \times135$$^{(9)}$  & 0.03$^{(7)}$          
	& $3\times 10^5$  & $2\times 10^3$ & $2\times 10^1$  & $6\times 10^{-2}$ \\ 
&&&&&&&&   $1\times 10^6$& $4\times 10^3$	&  $9\times 10^1$& $2\times 10^{-1}$\\
30 Doradus     & $>$400$^{(22)}$  & 2$^{(17)}$    & 50                       & 40$^{(25)}$&       & 200$^{(25)}$        & 0.09$^{(27)}$        
	& $2\times 10^5$ & $1\times 10^3$& $2\times 10^1$  & $6\times 10^{-2}$\\ 
&&&&&&&&  $2\times 10^6$ & $7\times 10^3$&  $2\times 10^2$& $3\times 10^{-1}$ \\	
N11 & 130 & 5$^{(26)}$  & 50      & $15\times 30$$^{(18)}$ &&
 $100\times 150^{(9)}$ &  0.08$^{(15)}$        
	& $9\times 10^4$  & $9\times 10^2$& $8\times 10^0$  & $3\times 10^{-2}$ \\ 
&&&&&&&&   $4\times 10^6$& $2\times 10^4$&  $4\times 10^2$& $8\times 10^{-1}$\\	
	\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{$N_{\star}$ is the number of stars with mass $\ge$$8~M_{\odot}$ (a Salpeter IMF has been assumed, expected for N11 where an index of 2.4 has been used).}
\tablefoottext{b}{Sizes are either the diameter if the region is spherical, or the large and small semi-axis if the region is ellipsoidal.} 
\tablefoottext{c}{The density is the Hydrogen nuclei density.} 
\tablefoottext{d}{Estimates of $\theta_{\star}$ are calculated from Eq.~(\ref{eq:Theta_ref}), as explained in Sect.~\ref{sec:selection}. The range of values of $\theta_{\star}$ given for each object and for each magnetic configuration reflects uncertainties in the actual values of bubble density, accelerator size and turbulence scale.}} 
\vspace*{-3mm}
\tablebib{(1)~\cite{Brandner2008a}; (2)~\cite{Brown1994a}; (3)~\cite{Brown1995a}; (4)~\cite{Burrows1993a}; (5)~\cite{Cash1980a}; 
(6)~\cite{Conti2004a}; (7)~\cite{Cooper2004a}; (8)~\cite{Davidson1997a}; (9)~\cite{Dunne2001a}; (10)~\cite{Hanson2003a}; 
(11)~\cite{Knodlseder2000a}; (12)~\cite{Knodlseder2002a}; (13)~\cite{Kothes2007a}; (14)~\cite{Lozinskaya1998a}; (15)~\cite{Maddox2009a}; 
(16)~\cite{Massey1995a}; (17)~\cite{Massey1998a}; (18)~\cite{Naze2004a}; (19)~\cite{Nichols-Bohlin1993a}; (20)~\cite{Oey1998a}; 
(21)~\cite{Rauw2007a}; (22)~\cite{Selman1999a}; (23)~\cite{Smith2000a}; (24)~\cite{Tsujimoto2007a}; (25)~\cite{Walborn1991a}; 
(26)~\cite{Walborn1992a}; (27)~\cite{Wang1991a}.} 
\vspace*{5mm} 
\end{table}