\begin{table}%ta.3continued %\centering \par \caption{\label{tab:grasilres}Properties of SMGs derived from the SED modeling.} \begin{tabular}{cc rrrrr rrcc crc c l} \hline\hline \noalign{\smallskip} & & \multicolumn{4}{c}{SFR ($M_\odot$ yr$^{-1}$)} & SSFR & $\log M_*$ & $M_{\rm burst}/M_*$ & $M_*/L_K$ & $\log M_{\rm d}$ & $\log L_{\rm IR}$ & $T_{\rm d}$ & $A_V$ & & \\ \cline{3-6} SMG & $z$ & SED & UV & IR & radio & (Gyr$^{-1}$) & ($M_\odot$) & (\%) & ($M_\odot/L_\odot$) & ($M_\odot$) & ($L_\odot$) & (K) & (mag) & $q$ & AGN? \\ (1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) & (10) & (11) & (12) & (13) & (14) & (15) & (16)\\ \hline \object{SMMJ163658.78+405728.1} & 1.190 & 129 & 8.41 & 171 & 274 & 0.56 & 11.49 & 0.9 & 0.59 & 9.13 & 11.10 & 24.4 & 1.14 & 2.31 & \dots\\ \object{SMMJ163704.34+410530.3} & 0.840 & 205 & 2.50 & 157 & 74 & 2.22 & 10.85 & 13.1 & 0.92 & 9.13 & 11.96 & 33.2 & 2.43 & 2.84 & \dots\\ \object{SMMJ163706.51+405313.8} & 2.374 & 2020 & 9.63 & 1478 & 1344 & 1.83 & 11.91 & 10.9 & 0.76 & 9.06 & 12.94 & 45.1 & 1.99 & 2.56 & spec\\ \object{SMMJ221724.69+001242.1} & 0.510 & 154 & 14.71 & 43 & 62 & 0.21 & 11.31 & 3.4 & 0.63 & 9.36 & 11.40 & 15.9 & 0.69 & 2.36 & \dots\\ \object{SMMJ221725.97+001238.9} & 3.094 & 2499 & 2.29 & 1935 & 1353 & 2.10 & 11.96 & 12.5 & 1.58 & 9.38 & 13.05 & 38.7 & 3.27 & 2.67 & \dots\\ \object{SMMJ221733.02+000906.0} & 0.926 & 447 & 0.72 & 381 & 333 & 0.88 & 11.64 & 4.5 & 1.56 & 9.16 & 12.35 & 33.2 & 2.58 & 2.58 & \dots\\ \object{SMMJ221733.12+001120.2} & 0.652 & 31 & 2.77 & 59 & 62 & 0.28 & 11.33 & 4.7 & 1.79 & 9.13 & 11.54 & 21.8 & 1.27 & 2.49 & rad\\ \object{SMMJ221733.91+001352.1} & 2.555 & 875 & 17.73 & 731 & 954 & 0.78 & 11.97 & 3.8 & 0.79 & 9.01 & 12.63 & 38.7 & 1.69 & 2.40 & \dots\\ \object{SMMJ221735.15+001537.2} & 3.098 & 594 & 8.51 & 536 & 1627 & 2.28 & 11.37 & 10.0 & 0.68 & 8.94 & 12.49 & 38.7 & 1.93 & 2.03 & \dots\\ \object{SMMJ221735.84+001558.9} & 3.089 & 1969 & 7.43 & 1668 & 1450 & 6.49 & 11.41 & 35.0 & 0.30 & 8.35 & 12.99 & 71.5 & 2.98 & 2.58 & \dots\\ \object{SMMJ221737.39+001025.1} & 2.614 & 2991 & 13.32 & 2641 & 2484 & 7.05 & 11.57 & 37.1 & 0.29 & 8.47 & 13.19 & 71.5 & 2.70 & 2.54 & \dots\\ \object{SMMJ221804.42+002154.4} & 2.517 & 1474 & 15.50 & 1239 & 908 & 6.30 & 11.29 & 33.5 & 0.55 & 8.85 & 12.86 & 52.6 & 2.11 & 2.65 & mIR\\ \object{SMMJ221806.77+001245.7} & 3.623 & 8825 & 29.59 & 7774 & 11225 & 20.81 & 11.57 & 109.9 & 0.23 & 8.25 & 13.66 & 113.3 & 3.76 & 2.36 & rad\\ % %\hline \object{SMMJ030226.17+000624.5} & 0.080 & 3 & 0.06 & 2 & 4 & 0.07 & 10.53 & 0.4 & 1.08 & 8.28 & 10.11 & 11.4 & 0.33 & 2.24 & rad\\ \object{SMMJ030238.62+001106.3} & 0.276 & 14 & 0.04 & 36 & 44 & 59.74 & 8.78 & 113.3 & 0.36 & 8.32 & 11.32 & 25.5 & 4.22 & 2.43 & spec,rad\\ \object{SMMJ030244.82+000632.3} & 0.176 & 6 & 0.59 & 11 & 7 & 0.37 & 10.46 & 0.0 & 0.76 & 8.22 & 10.80 & 20.1 & 1.44 & 2.69 & \dots\\ \object{SMMJ123651.76+621221.3} & 0.298 & 6 & 0.12 & 14 & 7 & 1.02 & 10.13 & 0.9 & 0.98 & 8.91 & 10.90 & 13.3 & 1.93 & 2.79 & \dots\\ % %\hline \multicolumn{1}{r}{mean} & 2.002 & 1065 & 68.35 & 873 & 1429 & 3.51 & 11.71 & 15.6 & 0.75 & 9.02 & 12.71 & 40.1 & 2.03 & 2.34 & \dots \\ \multicolumn{1}{r}{median} & 2.148 & 825 & 6.78 & 659 & 1087 & 1.72 & 11.54 & 7.2 & 0.68 & 8.91 & 12.58 & 38.7 & 1.99 & 2.40 & \dots \\ \multicolumn{1}{r}{std dev} & 0.851 & 1271 & 395.38 & 1066 & 1731 & 7.44 & 0.55 & 23.2 & 0.36 & 0.36 & 0.60 & 18.3 & 0.95 & 0.34 & \dots \\ \multicolumn{1}{r}{min} & 0.080 & 3 & 0.04 & 2 & 4 & 0.04 & 8.78 & 0.0 & 0.18 & 8.14 & 10.11 & 11.4 & 0.00 & 1.24 & \dots \\ \multicolumn{1}{r}{max} & 3.623 & 8825 & 3387.93 & 7774 & 11225 & 59.74 & 12.44 & 113.3 & 1.79 & 9.90 & 13.66 & 113.3 & 4.38 & 2.97 & \dots \\ \hline \end{tabular} \tablefoot{Column~(1):~SMG name. Column~(2):~redshift \citep{chapman05}. Column~(3):~total star formation rate (SFR) for 0.15--120~$M_\odot$ stars averaged over the last 50~Myr derived from the SED model. Column~(4):~SFR from UV emission interpolated from the SED template \citep[using][]{kennicutt}. Column~(5):~SFR from IR emission (Column 12) used in all analysis throughout the paper \citep[using][]{kennicutt}. Column~(6):~SFR from radio emission derived directly from the radio data \citep[using][]{bell03}. Column~(7):~specific \mbox{SFR}~$\equiv \mbox{SFR}_{\rm IR}/M_*$. Column~(8):~stellar mass. Column~(9):~Ratio of the mass of gas converted to star during the recent starburst episode to the total stellar mass. There are values greater than 100\%, because the starburst episode is ongoing; 0\% means that non-starburst template was adopted. Column~(10):~stellar mass to light ratio (luminosity at rest-frame~$K$ was intepolated using the best SED model). Column~(11):~dust mass. Column~(12):~total 8--1000~$\mu$m infrared luminosity. Column~(13):~dust temperature. Column~(14):~Average extinction $A_V=2.5\log$($V$-band starlight unextinguished / $V$-band starlight observed). Column~(15):~IR-radio correlation parameter (Sect.~\ref{sec:firr}). Column~(16):~AGN flag -- X: \mbox{X-ray} identified AGN; SB: X-ray identified starburst \citep{alexander05}; spec: spectroscopically identified AGN or QSO \citep{chapman05}; mIR: mid-IR identified AGN (Sect.~\ref{sec:agn}); rad: radio datapoint is more than 3$\sigma$ above the starburst model (Sect.~\ref{sec:agn}). The horizontal line divides the $z>0.5$ and $z<0.5$ samples. %This table is available in a machine-readable form in the electronic edition of the Journal } \end{table}