\begin{table}%t2
\par
\caption{\label{7:tab:source}The sample of sources observed with CHAMP+.}
\small
%\centerline
 {
\begin{tabular}{l l l l l l l l}  
\hline \hline
Source & RA & Dec & D & $L_{\rm{bol}}$ & $T_{\rm{bol}}$ & Class   \\
 & (J2000) & (J2000) & (pc)& ($L_{\rm{\odot}}$) & (K) &   \\ \hline
NGC 1333 IRAS 2	& 03:28:55.2& +31:14:35  & 250 & 12.7 & 62  & 0  \\    % in PERS
L1551 IRS 5     & 04:31:34.1&+18:08:05.0 & 160 & 20   & 75  & 1 \\
TMR 1		& 04:39:13.7& +25:53:21  & 140 & 3.1 & 133  & 1 \\  %
HH 46		& 08:25:43.8& --51:00:35.6& 450 & 16 & 102   & 1  \\ %  done as DC267.4-7.5
Ced 110 IRS 4	& 11:06:47.0& --77:22:32.4& 130 & 0.8 & 55   & 1 \\      %in CHAM
BHR 71		& 12:01:36.3& --65:08:44  & 200 & 11 & 60    & 0 \\ % done as DC297.7-2.8
IRAS 12496-7650	& 12:53:17.2& --77:07:10.6& 250 & 24 &326$^b$& 1  \\        %  in CHAM
RCrA IRS 7A$^c$	& 19:01:55.2& --36:57:21.0& 170 & -- & --   & 0   \\%    SMM 1C(nutter)/VLA10B
\hline 
& Sett.$^{a}$ & \multicolumn{2}{l}{Ref. Cont.} & \multicolumn{3}{l}{Ref. CO} \\  
NGC 1333 IRAS 2	& A   & \multicolumn{2}{l}{1, 2, 3, 4, 5, 6, 7}   & vii \\
L1551 IRS 5     & A   & \multicolumn{2}{l}{2, 8, 9, 10, 11, 12}  & i \\
TMR 1		& AB  & \multicolumn{2}{l}{13, 14, 15, 16}     & i \\
HH 46		& ABC & \multicolumn{2}{l}{1, 17, 18}         & ii, iii \\
Ced 110 IRS 4	&  AB & \multicolumn{2}{l}{7,19,20,21,22}   & iii, iv \\
BHR 71		&  AB & \multicolumn{2}{l}{17, 23, 24, 25}     & v \\
IRAS 12496-7650	& AB  & \multicolumn{2}{l}{26, this work}   & iii, viii\\
RCrA IRS 7A$^c$	& A   & \multicolumn{2}{l}{1, 7, 27, 28}       & iii, viii\\ \hline
\end{tabular}}
\par
\medskip
$^a$ Observed settings with CHAMP+. See Table \ref{7:tab:settings}. \\
$^b$ IRAS~12496-7650 is  likely to be viewed face-on and thus has strong IR emission and a high $T_{\rm{bol}}$. See van Kempen et~al. (2009, submitted).\\
$^c$ RCrA IRS 7 is a binary. Pointing was chosen to be on RCrA IRS 7A, believed to be the main embedded source, following results from van~Kempen et~al. (2009, submitted)
 and \citet{Groppi07}. RCrA IRS 7B is located 15\arcsec\ to the east.  At mid- and far-IR wavelengths, the source is heavily confused with RCrA. Therefore, no reliable $T_{\rm{bol}}$ and $L_{\rm{bol}}$ could be derived. \\
{Continuum References: }
1: \citet{diFrancesco08} 
2: \citet{Motte01} 
3: \citet{Gutermuth08}
4: \citet{Enoch06} 
5: \citet{Hatchell07} 
6: \citet{Sandell01}
7: \citet{Froebrich05}
8: \citet{Chandler00}
9: \citet{Reipurth02}
10: \citet{Osorio03}
11: \citet{Liu96}
12: \citet{Butner91}
13: \citet{Kenyon94}
14: \citet{Hogerheijde99}
15: \citet{Furlan08}
16: \citet{Terebey93}
17: \citet{Henning98}
18: \citet{vanKempen09}
19: \citet{Reipurth93}
20: \citet{Luhman08}
21: \citet{Lehtinen01}
22: \citet{Lehtinen03}
23: \citet{Evans07}
24: \citet{Bourke97}
25: \citet{Bourke01}
26: \citet{Henning93}
27: \citet{Nutter05}
28: \citet{Groppi07}\\
{CO references: }
i: \citet{Hogerheijde98},
ii: van~Kempen et~al. (2009, submitted),
iii: Paper I,
iv: \citet{Hiramatsu07}, 
v: \citet{Parise06},
vi: \citet{Knee00},
vii: \citet{Giannini01},
viii: \citet{Giannini99}. 
\vspace*{4mm}\end{table}