\begin{table}%t7
\caption{\label{t2mass}2MASS sources associated with the centimeter and/or millimeter emission toward the star-forming region IRAS~00117+6412.}
\par
%\scriptsize
\small
%\centerline
{\begin{tabular}{lccccccccc}
\hline\hline\noalign{\smallskip}
&2MASS
&\multicolumn{2}{c}{Position}
&
&
&
&$J-H$
&$H-K_{{\rm S}}$
\\
%\cline{3-4}
%\noalign{\smallskip}
Source
&Identification
&$\alpha (\rm J2000)$
&$\delta (\rm J2000)$
&$J$
&$H$
&$K_{{\rm S}}$
&color\tablefootmark{a}
&color\tablefootmark{a}
&IR$_{\rm excess}$\tablefootmark{b}
\\
\hline
\noalign{\smallskip}
\uchii\ 	&$00142828+6428471$	&00 14 28.29	&64 28 47.19
		&$14.94\pm0.08$	        &$13.28\pm0.07$	&$12.14\pm0.05$	 &$1.66$   &$1.14$  &$+0.18$	\\
%------------
MM1		&$00142616+6428444$	&00 14 26.16	&64 28 44.44	
		&$15.49\pm0.07$	        &$13.58\pm0.06$	&$12.22\pm0.04$	 &$1.91$   &$1.37$  &$+0.27$	\\
%------------
{\scriptsize 2M0014256}	&$00142558+6428416$	&00 14 25.59	&64 28 41.70 
                &$16.71\pm0.14$         &$14.35\pm0.05$ &$13.27\pm0.04$	 &$2.36$   &$1.09$  &$-0.27$	\\
\hline
\end{tabular}}
\par
\tablefoot{\tablefoottext{a}{Uncertainties in the colors are typically $\sim$$0.09$~mag.}
\tablefoottext{b}{The infrared excess is measured as the difference
between the $(H-K_{{\rm S}})$ color and the $(H-K_{{\rm S}})$ color corresponding to a
reddened main-sequence star (following the reddening law of Rieke \&
Lebofsky \cite{riekelebofsky1985}), \ie\ ${\rm IR_{excess}}=(H-K_{{\rm S}})-0.576\times(J-K_{{\rm S}})$.}}
\end{table}