\begin{table}%t4
\caption{\label{table:tab4}Best fitting parameters for the MIPS-d~sample.}
\small%\centerline
 {
\begin{tabular}{llllllllll}
\hline \hline
%&&&&&&&&&&& \\[-8pt]
ID&$z_{\rm phot}$&$\chi^2_{\nu}$&$P_{\chi^2_{\nu}}$&$A_{V}$&$z_{\rm inf-90\%}$&$z_{\rm sup-90\%}$&$z_{\rm 2-phot}$&$P_{\chi^2_{\nu},2}$ & log $M$\\
%&&&&&&&&&&& \\[-8pt]
\hline
\#588 &  4.285 &  0.785 &  64.36  & 0.60 & 3.690 &   4.740 &  9.388 &	0.05 &  9.973 \\
\#702 &  8.814 &  0.067 &  99.99  & 0.40 & 1.450 &  10.060 &  3.340 &  99.99 & 10.563 \\
\#1720 &  3.522 &  0.526 &  87.33  & 0.60 & 2.850 &   4.250 &  3.921 &  84.30 & 10.399 \\
\#2172 &  3.711 &  0.536 &  86.56  & 0.70 & 3.550 &   4.180 &  4.117 &  70.42 & 11.097 \\
\#2560 &  3.830 &  0.044 & 100.00  & 0.40 & 2.780 &   8.520 &  7.274 & 100.00 & 10.762 \\
\#2796 & 10.060 &  0.279 &  98.59  & 0.80 & 3.360 &  10.060 &  3.536 &  95.36 & 10.870$^{{a}} $ \\
\#2894 &  3.893 &  0.628 &  79.14  & 0.70 & 2.990 &   4.460 & 10.060 &	0.37 & 10.441 \\
\#3393 &  5.503 &  0.477 &  90.59  & 0.80 & 3.830 &   5.860 &  5.167 &  84.73 & 10.647 \\
\#3850 &  4.166 &  0.063 & 100.00  & 0.70 & 3.410 &   9.290 &  8.009 &  99.90 & 10.940\\
\#5157 &  4.740 &  0.344 &  96.90  & 0.00 & 4.110 &   7.400 &  6.504 &  92.59 & 11.433\\
\#5367 &  4.355 &  0.494 &  89.51  & 0.80 & 3.900 &   4.880 & 10.060 &	0.03 & 10.806\\
\#5511 &  4.152 &  2.521 &   0.50  & 0.50 & 4.040 &   4.250 &  1.310 &	0.00 & 10.551\\
\#6099 &  5.251 &  0.367 &  96.10  & 0.10 & 3.200 &   8.450 &  4.999 &  96.02 & 11.178\\
\#6245 &  5.062 &  0.108 &  99.98  & 0.00 & 4.460 &   5.370 &  2.934 &  81.31 & 10.662\\
\#6463 &  9.437 &  0.193 &  99.68  & 0.10 & 3.690 &  10.060 &  4.215 &  99.64 &  9.973$^{{a}} $\\
\#8520 &  3.683 &  0.573 &  83.71  & 0.00 & 3.340 &   3.830 &  3.137 &  44.99 & 10.730\\
\#9007 &  3.669 &  1.117 &  34.42  & 0.60 & 2.780 &   4.110 &  2.969 &  34.41 & 10.824\\
\#9301 &  8.226 &  0.059 & 100.00  & 0.20 & 2.640 &  10.060 &  8.037 & 100.00 & 11.035\\
\#9306 &  8.660 &  0.127 &  99.95  & 0.80 & 2.360 &  10.060 &  8.219 &  99.92 & 11.011\\
\#9782 &  3.928 &  1.472 &  14.28  & 0.20 & 3.480 &   4.320 &  8.723 &	0.02 & 11.116\\
\#10176 &  5.818 &  0.002 & 100.00  & 0.20 &3.550  &  9.570 &  5.517 & 100.00 & 11.280\\
\#11304 &  4.145 &  0.378 &  95.67  & 0.80 &3.550  &  8.100 &  5.461 &  89.78 & 10.759\\
\#12699 &  3.543 &  1.760 &   6.21  & 0.30 &3.200  &  3.690 &  3.354 &   5.62 & 10.558\\
\#13129 &  7.960 &  0.030 & 100.00  & 0.20 &3.410  & 10.060 &  8.296 & 100.00 & 11.056\\
\#13857 &  3.746 &  0.863 &  56.74  & 0.10 &3.270  &  4.040 &  3.403 &  43.23 & 10.707\\
\#14505 &  3.564 &  0.014 & 100.00  & 0.80 &2.920  & 10.060 &  7.757 & 100.00 & 10.025\\
\#14668 &  4.600 &  0.209 &  99.56  & 0.10 &1.870  &  5.230 &  4.789 &  99.53 & 10.177\\
\#14722 &  4.145 &  1.816 &   5.23  & 0.40 &4.110  &  4.180 &  0.617 &   0.36 & 10.180\\
\#14793 &  4.474 &  1.225 &  27.41  & 0.00 &4.040  &  5.160 &  9.185 &   0.01 & 11.411\\
\#15541 &  3.949 &  1.216 &  27.45  & 0.40 &3.690  &  4.110 &  0.680 &   0.00 & 11.146\\
\#15761 &  4.292 &  0.177 &  99.78  & 0.10 &3.900  &  4.530 &  6.567 &   0.00 & 11.126\\
\#15771 &  3.564 &  0.360 &  96.35  & 0.20 &3.060  &  3.830 &  6.854 &   0.00 & 11.283\\
\hline
\end{tabular}}
\medskip
See Table~\ref{table:tab3} for the column description. For the objects with extremely high redshift best fit solutions, the same caveat we gave in Table~\ref{table:tab3} should be taken into account. \\
$^{{a}}$ These values for the galaxy masses were found for the secondary solutions of photometric redshift, because the \textit{hyperzmass} software did not find a acceptable solution at $z\sim 9{-}10$.
\end{table}