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\def\ub{\underbar{~}}
\def\decsec{\hbox{$^{\prime\prime}\hskip-3pt .$}}
\def\sec{$^{\prime\prime}$}
\def\sfr{\rm M_{\odot}\ yr^{-1}}
\def\kmsmpc{{\rm km\ s^{-1}Mpc^{-1}}}
\def\exp#1{\times 10^{#1}}
\def\etal{{\it et al.}}
\def\lya{Ly$\alpha$}
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\begin{deluxetable}{lcccccccl}
\tablenum{2}
\tablecolumns{9}
\tablewidth{636pt}
%\tablewidth{0pc}
\scriptsize
\tablecaption{Confirmed Redshifts in the HDF}
%
\tablehead{
\colhead{Name}  & 
\colhead{$z$ \tablenotemark{a}} &
\colhead{$Q_z$ \tablenotemark{b}} &
\multicolumn{2}{c}{$r_{1/2}$ \tablenotemark{c}} & 
\colhead{$M_B$ \tablenotemark{d}} & 
\colhead{SFR \tablenotemark{e}} & 
\colhead{$W_0(\rm{Ly}\alpha)$ \tablenotemark{f}} &
\colhead{Ref \tablenotemark{g}} \\
\cline{4-5}\\
\colhead{} &
\colhead{} &
\colhead{} &
\colhead{(\sec) } &
\colhead{($h_{50}^{-1}$ kpc)} &
\colhead{} &
\colhead{($h_{50}^{-2} \sfr$)} &
\colhead{(\AA)} &
\colhead{}
}

\startdata
hd4\ub1229\ub1791 &  0.483 &  3 &   0.53  &   4.15 &  -17.11 &   0.14\tablenotemark{h} &  \nodata   & L4-515\nl                       
hd2\ub2030\ub0287 &  2.267 &  4 &   0.36  &   4.37 &  -22.19 &  20.80 &   34.1   & L2-14/M2-82.1/SC2-02\nl         
hd2\ub1410\ub0259 &  3.160 &  3 &   0.37  &   4.50 &  -22.16 &  14.36 &    6.2   & L2-5?/C2P1/SC2-01 \nl           
hd4\ub0367\ub0266 &  2.931 &  4 &   0.58  &   7.13 &  -22.66 &  17.36 &  \nodata & L4-3* \nl                        
                  &        &    &(0.35, 0.44)&(4.29, 5.37)&(-22.55, -22.23)&        & \nl
hd4\ub2030\ub0851 &  2.980 &  3 &   0.27  &   3.33 &  -22.34 &  14.52 &  \nodata & L4-200*/M4-363.0/SC4-04 \nl      
hd3\ub0408\ub0684 &  3.233 &  4 &   0.21  &   2.53 &  -22.49 &  17.16 &   22.1   & L3-120*\nl                       
hd2\ub0698\ub1297 &  3.430 &  4 &   0.45  &   3.07 &  -22.85 &  23.76 &   14.5   & L2-310*\nl                       
                  &        &    &(0.22, 0.22)&(2.67, 2.72)&(-22.12, -21.99)& &      & \nl
hd2\ub0705\ub1366 &  3.368 &  4 &   0.14  &   1.75 &  -22.67 &  22.36 &   11.9   & L2-331*/M2-637.0/SC2-11 \nl      
hd2\ub1918\ub1912 &  star  &\nodata& \nodata  & \nodata  &  \nodata  &  \nodata &  \nodata   & L2-526/SC2-14\nl         
hd2\ub0434\ub1377 &  2.991 &  4 &   0.34  &   4.13 &  -22.83 &  20.72&  \nodata  & L2-334*/C2P2/M2-643.0/SC2-12 \nl 
                  &        &    &(0.16, 0.17)&(1.95, 2.06)&(-22.15, -21.96)&         &  \nl
hd2\ub1359\ub1816 &  3.181 &  4 &   0.32  &   3.90 &  -22.99 &  24.92 &  \nodata & L2-495*\nl                       
hd2\ub0624\ub1688 &  2.419 &  4 &   0.31  &   3.83 &  -21.60 &   6.56 &    9.3   & L2-445/M2-824.0 \nl             
                  &        &    &(0.26, 0.16)&(3.17, 1.96)&(-21.35, -20.40)&        & \nl
hd2\ub0725\ub1818 &  2.233 &  4 &   0.26  &   3.21 &  -22.10 &  16.96 &  \nodata   & L2-496/M2-903.0/SC2-12 \nl      

\enddata

\tablenotetext{a}{Redshift.}  \tablenotetext{b}{Redshift quality.
3=redshift probable, with two or more spectral features identified;
4=redshift definite, with multiple spectral features identified.}
\tablenotetext{c}{Half-light radius in arcsec measured from the
``drizzled'' images, and in kpc calculated assuming $H_0=50\ \kmsmpc,
q_0=0.05$.  Pairs of values in parentheses indicate subclumps for the
preceding object.  Values have not been corrected for the WFPC2 PSF
FWHM$\sim$ 0\decsec14; such a correction will make the median
half-light radius 10\% smaller, but will have a much larger effect on
the smallest sources.  For $q_0=0.5$, values would be $\sim$ 0.6 times
those listed here. } \tablenotetext{d}{Absolute $B$ magnitude
calculated from the observed $I814$ magnitude converted to Vega-based
($I_{814,Vega} = I_{814,ST} - 1.258$) and assuming $k-$corrections for
a blue star-forming galaxy and $H_0=50\ \kmsmpc, q_0=0.05$.  Pairs of
values indicate subclumps for the preceding object, corrected by 0.1
mag (fainter) to account for the average additional flux in the {\em
total} object we measure compared to the STScI HDF FOCAS catalog.}
\tablenotetext{e}{Star formation rate calculated assuming
$SFR=L_{\lambda}(1216)/1\exp{40} \sfr$ or
$SFR=L_{\lambda}(1500)/1\exp{40.1} \sfr$, for $H_0=50\ \kmsmpc,
q_0=0.05$.  For $H_0=100\ \kmsmpc, q_0=0.5$, values will be a factor
of $\sim 11$ times lower.}  \tablenotetext{f} {Rest equivalent width
of \lya\ emission line.}  \tablenotetext{g} {Other published candidate
lists in which object appears: C=Clements \& Couch (1996); L=Lanzetta
\etal\ (1996); M=Madau \etal\ (1996); S=Steidel \etal\ (1996b).  For
Lanzetta \etal\, a * indicates that the predicted redshift was
$z>2.2$.}  \tablenotetext{h} {SFR derived from [O~II] emission line,
assuming $SFR=2.4\times10^{-12} \times EW(O~II) \times {\rm exp}
(-0.4(M_B - {\rm M}_{\odot,B}))$ (Guzm\'an \etal\ 1996).}

\end{deluxetable}
\end{document}