\begin{table} 
\caption{IR fluxes, star formation rates and derived dust attenuation. }
\small%\centerline
{
\begin{tabular}{@{}lcccccccc}
\hline
\hline
\multicolumn{8}{c}{$z = 2.3$} \\
\hline
LAE\_ & $F_{24~\mu{\rm m}}$ & $L_{\rm IR}$ &  $L_{\rm bol}$ & ${\it SFR}_{\rm bol}$ & $A_{1600}$ & Offset & Remark \\
COSMOS\_\# & $\mu$Jy & erg s$^{-1}$ & erg s$^{-1}$ & $M_{\odot}$ yr$^{-1}$ & & arcsec &  &  \\
\hline
  20 & $154\pm16$ &  $46.50\pm0.05$ & $46.50\pm0.07$ & $  1420\pm220   $ & $5.51\pm0.18$ & 1.49 & AGN \\
  36 & $835\pm20$ &  $47.69\pm0.02$ & $47.69\pm0.02$ & $ 21830\pm1000  $ & $7.65\pm0.05$ & 0.19 & AGN \\
  42 & $155\pm47$ &  $46.50\pm0.13$ & $46.51\pm0.19$ & $  1460\pm510   $ & $3.89\pm0.45$ & 0.82 & AGN \\
  52 & $289\pm41$ &  $46.94\pm0.08$ & $46.94\pm0.10$ & $  3920\pm780   $ & $6.90\pm0.24$ & 0.56 & AGN \\
  94 & $132\pm87$ &  $46.39\pm0.19$ & $46.39\pm0.38$ & $  1100\pm640   $ & $7.13\pm0.95$ & 1.28 &     \\
  96 & $88\pm46$ &   $46.10\pm0.17$ & $46.11\pm0.30$ & $   570\pm390   $ & $5.03\pm0.74$ & 3.83 &     \\
  101 & $259\pm17$ & $46.86\pm0.04$ & $46.86\pm0.06$ & $  3280\pm440   $ & $7.31\pm0.16$ & 0.09 & AGN \\
  108 & $143\pm18$ & $46.44\pm0.07$ & $46.45\pm0.08$ & $  1270\pm230   $ & $3.96\pm0.21$ & 0.39 & AGN \\
  115 & $202\pm16$ & $46.69\pm0.05$ & $46.69\pm0.05$ & $  2210\pm260   $ & $4.83\pm0.13$ & 0.06 & AGN \\
  126 & $181\pm25$ & $46.61\pm0.08$ & $46.62\pm0.09$ & $  1880\pm360   $ & $3.73\pm0.22$ & 0.44 & AGN \\
  129 & $182\pm14$ & $46.61\pm0.05$ & $46.62\pm0.06$ & $  1860\pm230   $ & $5.91\pm0.14$ & 0.29 & AGN \\
  130 & $75\pm11$ &  $45.99\pm0.08$ & $46.00\pm0.11$ & $   450\pm100   $ & $5.45\pm0.27$ & 0.56 & AGN \\
  140 & $509\pm19$ & $47.34\pm0.02$ & $47.34\pm0.03$ & $  9790\pm670   $ & $7.36\pm0.08$ & 0.15 & AGN \\
  150 & $297\pm16$ & $46.96\pm0.03$ & $46.96\pm0.05$ & $  4090\pm420   $ & $7.12\pm0.12$ & 0.35 & AGN \\
  151 & $404\pm11$ & $47.18\pm0.02$ & $47.18\pm0.04$ & $  6740\pm610   $ & $8.01\pm0.10$ & 0.45 & AGN \\
  152 & $90\pm13$ &  $46.12\pm0.08$ & $46.13\pm0.10$ & $   610\pm120   $ & $3.95\pm0.23$ & 2.73 &     \\
  155 & $190\pm11$ & $46.64\pm0.04$ & $46.66\pm0.04$ & $  2040\pm180   $ & $3.79\pm0.10$ & 0.37 & AGN \\
  162 & $111\pm11$ & $46.26\pm0.06$ & $46.26\pm0.11$ & $   830\pm180   $ & $6.69\pm0.27$ & 2.75 &     \\
  167 & $216\pm18$ & $46.73\pm0.05$ & $46.74\pm0.06$ & $  2440\pm340   $ & $6.66\pm0.16$ & 3.09 &     \\
  171 & $123\pm11$ & $46.34\pm0.05$ & $46.34\pm0.06$ & $   990\pm130   $ & $4.61\pm0.15$ & 0.70 &     \\
  173 & $197\pm14$ & $46.67\pm0.04$ & $46.68\pm0.05$ & $  2130\pm220   $ & $4.75\pm0.12$ & 1.05 & AGN \\
  175 & $277\pm16$ & $46.91\pm0.04$ & $46.91\pm0.05$ & $  3660\pm400   $ & $7.13\pm0.13$ & 0.44 & AGN \\
  179 & $352\pm190$ & $47.08\pm0.18$ & $47.08\pm0.31$ & $  5390\pm2750 $ & $7.83\pm0.77$ & 0.25 &     \\
  183 & $95\pm11$ &  $46.16\pm0.07$ & $46.16\pm0.08$ & $   660\pm110   $ & $4.80\pm0.20$ & 0.81 &     \\
  187 & $82\pm11$ &  $46.05\pm0.07$ & $46.05\pm0.09$ & $   510\pm100   $ & $4.41\pm0.22$ & 2.62 &     \\
\hline
\multicolumn{8}{c}{$z = 0.3$} \\
\hline
ID & $F_{8~\mu{\rm m}}$   &  $L_{\rm IR}$ &  $L_{\rm bol}$ & ${\it SFR}_{\rm bol}$ & $A_{1600}$ & --  & Remark & \\
    & $\mu$Jy & erg s$^{-1}$ & erg s$^{-1}$ & $M_{\odot}$ yr$^{-1}$ &  &  \\
\hline
CDFS\_1348  & $1.63\pm0.03$  & $45.19\pm0.01$ & $45.20\pm0.01$ & $   71\pm2   $ & $4.91\pm0.03$ & & & \\
CDFS\_1821  & $0.38\pm0.05$  & $44.17\pm0.08$ & $44.20\pm0.09$ & $    7\pm1   $ & $2.69\pm0.21$ & & & \\
CDFS\_2422  & $10.72\pm0.04$ & $46.52\pm0.01$ & $46.52\pm0.01$ & $ 1480\pm10  $ & $7.52\pm0.01$ & & Unclass. & \\
CDFS\_3801  & $0.64\pm0.06$  & $44.53\pm0.06$ & $44.54\pm0.07$ & $   16\pm2   $ & $3.57\pm0.16$ & & & \\
CDFS\_4927  & $0.70\pm0.03$  & $44.60\pm0.03$ & $44.61\pm0.03$ & $   18\pm1   $ & $4.14\pm0.08$ & & & \\
CDFS\_5007  & $0.46\pm0.09$  & $44.31\pm0.09$ & $44.32\pm0.12$ & $    9\pm2   $ & $3.45\pm0.28$ & & & \\
CDFS\_5448  & $1.56\pm0.05$  & $45.16\pm0.02$ & $45.16\pm0.02$ & $   66\pm3   $ & $5.20\pm0.05$ & & & \\
CDFS\_6523  & $1.34\pm0.04$  & $45.05\pm0.02$ & $45.06\pm0.02$ & $   51\pm2   $ & $4.98\pm0.05$ & & & \\
CDFS\_6535  & $2.36\pm0.05$  & $45.45\pm0.01$ & $45.46\pm0.01$ & $  130\pm4   $ & $5.44\pm0.04$ & & & \\
CDFS\_7100  & $1.27\pm0.06$  & $45.01\pm0.03$ & $45.02\pm0.03$ & $   47\pm3   $ & $4.87\pm0.08$ & & & \\
CDFS\_16104 & $0.33\pm0.06$  & $44.07\pm0.09$ & $44.13\pm0.12$ & $    6\pm2   $ & $2.12\pm0.25$ & & & \\
CDFS\_17033 & $0.44\pm0.07$  & $44.28\pm0.08$ & $44.29\pm0.10$ & $    8\pm2   $ & $3.38\pm0.23$ & & & \\
CDFS\_19355 & $5.33\pm0.06$  & $46.02\pm0.01$ & $46.03\pm0.01$ & $  478\pm8   $ & $6.02\pm0.02$ & & Unclass. & \\
CDFS\_21667 & $3.54\pm0.05$  & $45.74\pm0.01$ & $45.74\pm0.01$ & $  246\pm6   $ & $5.79\pm0.03$ & & & \\
CDFS\_21739 & $0.78\pm0.05$  & $44.67\pm0.04$ & $44.69\pm0.04$ & $   22\pm2   $ & $3.73\pm0.10$ & & Unclass. & \\
CDFS\_30899 & $0.37\pm0.04$  & $44.15\pm0.06$ & $44.18\pm0.07$ & $    7\pm1   $ & $2.78\pm0.16$ & & & \\
ELAISS1\_13715 & $2.90\pm0.20$  & $45.60\pm0.04$ & $45.60\pm0.05$ & $  179\pm18  $ & $5.51\pm0.11$ & & Unclass. & \\
ELAISS1\_16998 & $4.75\pm0.07$  & $45.94\pm0.01$ & $45.95\pm0.01$ & $  396\pm9   $ & $6.64\pm0.02$ & & & \\
ELAISS1\_6587  & $0.26\pm0.06$  & $43.89\pm0.10$ & $43.94\pm0.14$ & $    4\pm1   $ & $2.30\pm0.30$ & & AGN & \\
ELAISS1\_8180  & $17.72\pm0.04$ & $46.87\pm0.01$ & $46.87\pm0.01$ & $ 3340\pm10  $ & $7.82\pm0.01$ & & Unclass. & \\
ELAISS1\_21062 & $0.36\pm0.10$  & $44.13\pm0.13$ & $44.17\pm0.18$ & $    7\pm2   $ & $2.54\pm0.39$ & & & \\
ELAISS1\_23257 & $0.42\pm0.05$  & $44.23\pm0.06$ & $44.26\pm0.07$ & $    8\pm1   $ & $2.68\pm0.17$ & & Unclass. & \\
ELAISS1\_23425 & $0.17\pm0.05$  & $43.62\pm0.12$ & $43.78\pm0.18$ & $    3\pm1   $ & $1.16\pm0.27$ & & & \\
ELAISS1\_16921 & $1.93\pm0.05$  & $45.31\pm0.02$ & $45.31\pm0.02$ & $   93\pm4   $ & $5.07\pm0.05$ & & & \\
\hline
%\label{tab:IR}
\end{tabular}}
\smallskip
 Columns are: (1) flux in the 8/24~$\mu$m data; (2) infrared luminosity; (3) bolometric luminosity; (4) star formation rate; (5) dust attenuation derived from the infrared luminosities, (6) offsets between MIPS catalogue source and LAE candidate in z23 sample, and (7) other remarks. The IDs for the z03 sample are from Deharveng et~al. (2008). Full table is available in the online version.
\end{table}