\begin{table}%t1
%\centering
\par
\caption{\label{lineresults}Results of HIFI NH$_3$ and H$_2$O observations and NH$_3$ modeling.}
\par
\tiny\begin{tabular}{lcclcccccccc}
\hline \hline \noalign{\smallskip}
Object & $\alpha_{\rm J2000}$ & $\delta_{\rm J2000}$  &$D$&$\Mdot$$^{\rm Lit}$&$\varv$$_\infty$ & $\varv$$_{\rm LSR}$ range  &$\int T_{\rm MB}{\rm d}$$\varv$&$\Mdot$$^{\rm Mod}$&$r_{\rm out}$&$\theta_{\rm out}$&$X_{{\rm NH}_3}$\\
\hline\noalign{\smallskip}
&  &    &(kpc) &(\Mspy) &(km~s$^{-1})$   &(km~s$^{-1})$    &(K km~s$^{-1})$ &(\Mspy)&(cm) &($''$)\\
%\hline
IK Tau          & $03^{\rm h}53^{\rm m}28\fs8$  &$+11^\circ 24' 23''$ 
& 0.25\{1\}&$8\times10^{-6}$\{2\}&18 \{2\} & [11.5, 57.2] &  \d5.1 &
$8\times10^{-6}$&$5.0\times10^{15}$& 1.3&(1--3)~$10^{-6}$  \\
&                      &                      &&&&         [10.4, 59.5] & 10.3\\
VY CMa       & 07 22 58.3 &$-25$ 46 03 & 1.1 \{3\} &(0.8--3.4)~$10^{-4}$\{4\} &  35 \{4\}& [$-23.7$, 64.3] &15.5 &
								$1.8\times10^{-4}$&$3.5\times10^{16}$&2.1&$3~10^{-6}$\\ %/47 \{5\}
&                     &                       &&&&       [$-34$, 79]    & 51.2\\
OH26.5+0.6& 18 37 32.5 &$-$05 23 59 & 1.37 \{5\}  &$2.4\times10^{-4}$ \{5\} & 16 \{6\} &  [14.6, 43.2]  &\d0.96&
								 $2.4\times10^{-4}$       &$2.5\times10^{16}$&1.2&$3~10^{-7}$\\
&                    &                       &&&&        [15.0, 43.2]  &\d3.4 \\      
IRC+10420 & 19 26 48.1 &  +11   21 17& 5 \{7\}  &$8\times10^{-4}$ \{7\}      &   	38 \{7\}&[39,112]     & \d3.1&
								$2\times10^{-3}$        &$1.5\times10^{17}$      &2.0& (2--5)~$10^{-7}$\\ %/44 \{5\}
&  & &&&&        [42.8,116.4] &\d7.4\\
\hline
\end{tabular}
\tablefoot{Columns are (from left to right) the object, J2000 right 
ascension and declination of observed position, distance,  mass-loss rate from the literature, terminal expansion velocity (from CO data), FWZP LSR velocity range 
with observed emission, integrated main-beam brightness temperature, as well as mass-loss, outer radius of the NH$_3$ distribution (in cm and in arcsec),  and   [\nhhh/H$_2$] abundance ratio derived from our modeling. For the $\varv$$_{\rm LSR}$ range and $\int T_{\rm MB}{\rm d} \varv$  for each source, the first and second rows  give the values for the 
\nhhh\ and the H$_2$O lines, respectively. Numbers in braces relate to the following references for distances and mass loss rates: 
\{1\} \citet{Hale1997}; \{2\} \citet{Decin2010}; 
\{3\} \citet{Choi2008}; \{4\} \citet{Decin2006}; 
\{5\} \citet{Justtanont2006}; \{6\} \citet{Kemper2003};
\{7\} \citet{trung2009}.}
\vspace*{-3.6mm}
\end{table}