Table 6: Values of the baryonic masses, SFRs and bolometric IR ( $8 \div 1000~\mu$m) luminosities of the 15 $\mu $m sources in the HDF-S, as derived from the analysis of their spectral energy distributions (see Sects. 4.3 and 4.4).
Obj z $L_{\rm IR}$ SFR M M range
#   $L_\odot$ $[M_\odot\,\rm yr^{-1}]$ $[10^{11}M_\odot]$ $[10^{11}M_\odot]$
14 0.41 $5.8\times 10^{10}$ 10.0 0.32 $0.20\div0.40$
15 (0.55) $1.8\times 10^{11}$ 30.6 3.10 $2.30\div3.10$
16 0.62 $8.7\times 10^{10}$ 14.9 0.29 $0.21\div0.33$
18 (0.55) $1.4\times 10^{11}$ 23.4 5.20 $5.00\div5.50$
19 1.57 $1.4\times 10^{12\ast}$ - - -
20 0.39 $3.5\times 10^{10}$ 6.0 0.80 $0.55\div1.28$
23 0.46 $2.9\times 10^{11}$ 50.2 0.97 $0.42\div1.50$
25 0.58 $3.3\times 10^{11}$ 56.0 0.80 $0.50\div1.20$
27 0.58 $2.6\times 10^{11}$ 44.8 4.70 $3.90\div5.70$
28 0.58 $9.6\times 10^{10}$ 16.5 0.40 $0.25\div0.70$
30 (0.40) $2.7\times 10^{10}$ 4.6 0.01 $0.005 \div 0.020$
36 (0.65) $2.7\times 10^{11}$ 46.3 0.40 $0.20 \div 0.60$
38 1.39 $1.3\times 10^{12\ast}$ - 1.40 $1.00 \div 3.00$
39 1.27 $4.4\times 10^{12}$ 748.9 1.70 $1.00\div3.20$
40 1.27 $1.5\times 10^{12}$ 264.9 1.20 $0.70\div3.00$
41 (0.30) $1.6\times 10^{10}$ 2.7 0.055 $0.045\div 0.069$
43 0.95 $3.3\times 10^{11}$ 57.5 0.50 $0.20\div1.00$
45 (0.65) $3.9\times 10^{11}$ 66.6 0.80 $0.40\div1.60$
48 (0.30) $1.6\times 10^{10}$ 2.8 0.10 $0.06\div0.20$
52 (0.60) $1.2\times 10^{11}$ 20.1 0.13 $0.11\div0.16$
53 0.58 $2.2\times 10^{11}$ 38.5 1.20 $1.00\div1.50$
55 0.76 $2.6\times 10^{11}$ 45.4 1.30 $0.60\div1.60$
60 1.23 $9.7\times 10^{11}$ 167.2 2.50 $1.60\div4.00$
62 0.73 $2.2\times 10^{11}$ 36.9 0.66 $0.35\div0.90$
67 (1.00) $1.4\times 10^{12}$ 244.3 0.34 $0.21\div0.60$
71 (0.45) $2.6\times 10^{10}$ 4.4 0.04 $0.015\div 0.060$
72 0.55 $2.2\times 10^{11}$ 36.9 1.40 $1.10\div1.80$
73 0.17 $8.0\times 10^{10}$ 13.7 1.50 $0.90\div1.90$
75 (0.45) $1.5\times 10^{11}$ 25.0 1.30 $0.93\div1.60$
77 (0.40) $6.9\times 10^{10}$ 11.8 0.80 $0.48\div1.15$
79 0.74 $2.2\times 10^{11}$ 38.4 0.60 $0.30\div1.20$
82 0.69 $5.2\times 10^{11}$ 90.2 0.50 $0.22\div1.10$
85 (0.40) $2.8\times 10^{10}$ 4.7 5.70 $5.20\div6.00$

$^\ast$ Based on the AGN model described in Appendix A.

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