Table 1: Results of the stellar-mass estimate based of SEDs fitting. For each ISO/LW3 HDFS source we report redshift (Franceschini et al. 2003; photometric if within parenthesis, spectroscopic otherwise), total number of models produced by the spectrophotometric synthesis code (without the SIRTF constraints), effective number of SSPs contributing to best fit (for the optical+LW3 data, but without the SIRTF constraints), optical $\chi ^2$ and mass of the best fit solution. The last three columns report three different estimates of the mass uncertainties due to degeneracies: $\Delta M$ at 68.3% and 95.5% confidence levels (corresponding to 1 $\sigma$ and 2 $\sigma$ ) and 2 $\sigma$ mass range obtained simulating SIRTF/IRAC observations (only for some randomly selected sources).
Obj z $N_{\rm tot}$ $N_{\rm SSP}$ Mass (b.f.) $\chi^2_{\rm opt}$ $\Delta M_{1\sigma}$ $\Delta M_{2\sigma}$ $\Delta M_{\rm SIRTF}$

# mdls. b.f. $[10^{11}~M_\odot]$ b.f. $[10^{11}~M_\odot]$ $[10^{11}~M_\odot]$ $[10^{11}~M_\odot]$

S14 0.41 420 014 3 0.32 4.15 0.21-0.35 0.21-0.38

S15 (0.55) 451 212 2 3.10 13.55 2.97-3.29 2.61-3.49

S16 0.62 430 819 4 0.29 4.73 0.23-0.28 0.22-0.31

S18 (0.55) 202 806 4 5.20 14.37 5.13-5.47 4.62-5.67

S20 0.39 416 408 4 0.80 3.65 0.57-1.20 0.57-1.26

S23 0.46 409 213 4 0.97 8.16 0.45-1.16 0.41-1.64 0.60-1.20

S25 0.58 430 807 2 0.80 2.70 0.54-1.26 0.44-1.47 0.40-1.34

S27 0.58 507 625 4 4.70 4.56 4.44-5.62 3.71-5.68 4.17-5.54

S28 0.58 476 432 4 0.40 4.45 0.29-0.55 0.27-0.69

S30 (0.40) 206 401 3 0.01 3.88 0.005-0.007 0.005-0.025

S36 (0.65) 198 044 4 0.40 0.93 0.23-0.60 0.21-0.65

S40 1.27 385 289 4 1.20 8.71 1.43-2.01 0.89-3.05 0.80-2.00

S41 (0.30) 208 838 3 0.055 6.43 0.051-0.059 0.045-0.069

S43 0.95 409 212 4 0.50 0.77 0.25-0.87 0.22-0.94 0.21-0.77

S45 (0.65) 526 817 4 0.80 5.67 0.53-1.69 0.24-1.71 0.30-1.25

S48 (0.30) 210 015 3 0.10 4.08 0.14-0.21 0.058-0.21

S52 (0.60) 278 402 4 0.13 3.81 0.13-0.17 0.12-0.17

S53 0.58 506 477 3 1.20 3.34 0.99-1.38 0.99-1.52 1.20-1.38

S55 0.76 477 664 5 1.30 1.16 0.87-1.69 0.55-1.69 1.15-1.90

S60 1.23 492 090 4 2.50 14.38 1.91-2.89 1.75-6.23 2.00-3.20

S62 0.73 462 014 4 0.66 3.04 0.69-0.88 0.66-0.95

S67 (1.00) 424 812 4 0.34 12.12 0.21-0.87 0.21-0.91

S71 (0.45) 230 406 4 0.04 5.02 0.016-0.044 0.013-0.067

S72 0.55 421 227 3 1.40 12.39 1.14-1.30 1.12-2.01

S73 0.17 441 608 4 1.50 10.00 0.95-1.01 0.84-1.94 0.96-1.82

S75 (0.45) 222 010 4 1.30 4.19 1.16-1.36 0.83-1.40

S77 (0.40) 210 033 4 0.80 4.73 0.91-1.10 0.47-1.16 0.45-1.14

S79 0.74 499 221 3 0.60 1.60 0.65-1.18 0.30-1.21

S82 0.69 438 044 4 0.50 9.61 0.49-0.62 0.37-0.83 0.51-0.69

S85 (0.40) 414 053 3 5.70 25.77 5.51-5.79 4.78-6.19

**Table 1:** Results of the stellar-mass estimate based of SEDs fitting. For each ISO/LW3 HDFS source we report redshift (Franceschini et al. 2003; photometric if within parenthesis, spectroscopic otherwise), total number of models produced by the spectrophotometric synthesis code (without the SIRTF constraints), effective number of SSPs contributing to best fit (for the optical+LW3 data, but without the SIRTF constraints), optical $\chi ^2$ and mass of the best fit solution. The last three columns report three different estimates of the mass uncertainties due to degeneracies: $\Delta M$ at 68.3% and 95.5% confidence levels (corresponding to 1 $\sigma$ and 2 $\sigma$ ) and 2 $\sigma$ mass range obtained simulating SIRTF/IRAC observations (only for some randomly selected sources).
Obj	z	$N_{\rm tot}$	$N_{\rm SSP}$	Mass (b.f.)	$\chi^2_{\rm opt}$	$\Delta M_{1\sigma}$	$\Delta M_{2\sigma}$	$\Delta M_{\rm SIRTF}$
#		mdls.	b.f.	$[10^{11}~M_\odot]$	b.f.	$[10^{11}~M_\odot]$	$[10^{11}~M_\odot]$	$[10^{11}~M_\odot]$
S14	0.41	420 014	3	0.32	4.15	0.21-0.35	0.21-0.38
S15	(0.55)	451 212	2	3.10	13.55	2.97-3.29	2.61-3.49
S16	0.62	430 819	4	0.29	4.73	0.23-0.28	0.22-0.31
S18	(0.55)	202 806	4	5.20	14.37	5.13-5.47	4.62-5.67
S20	0.39	416 408	4	0.80	3.65	0.57-1.20	0.57-1.26
S23	0.46	409 213	4	0.97	8.16	0.45-1.16	0.41-1.64	0.60-1.20
S25	0.58	430 807	2	0.80	2.70	0.54-1.26	0.44-1.47	0.40-1.34
S27	0.58	507 625	4	4.70	4.56	4.44-5.62	3.71-5.68	4.17-5.54
S28	0.58	476 432	4	0.40	4.45	0.29-0.55	0.27-0.69
S30	(0.40)	206 401	3	0.01	3.88	0.005-0.007	0.005-0.025
S36	(0.65)	198 044	4	0.40	0.93	0.23-0.60	0.21-0.65
S40	1.27	385 289	4	1.20	8.71	1.43-2.01	0.89-3.05	0.80-2.00
S41	(0.30)	208 838	3	0.055	6.43	0.051-0.059	0.045-0.069
S43	0.95	409 212	4	0.50	0.77	0.25-0.87	0.22-0.94	0.21-0.77
S45	(0.65)	526 817	4	0.80	5.67	0.53-1.69	0.24-1.71	0.30-1.25
S48	(0.30)	210 015	3	0.10	4.08	0.14-0.21	0.058-0.21
S52	(0.60)	278 402	4	0.13	3.81	0.13-0.17	0.12-0.17
S53	0.58	506 477	3	1.20	3.34	0.99-1.38	0.99-1.52	1.20-1.38
S55	0.76	477 664	5	1.30	1.16	0.87-1.69	0.55-1.69	1.15-1.90
S60	1.23	492 090	4	2.50	14.38	1.91-2.89	1.75-6.23	2.00-3.20
S62	0.73	462 014	4	0.66	3.04	0.69-0.88	0.66-0.95
S67	(1.00)	424 812	4	0.34	12.12	0.21-0.87	0.21-0.91
S71	(0.45)	230 406	4	0.04	5.02	0.016-0.044	0.013-0.067
S72	0.55	421 227	3	1.40	12.39	1.14-1.30	1.12-2.01
S73	0.17	441 608	4	1.50	10.00	0.95-1.01	0.84-1.94	0.96-1.82
S75	(0.45)	222 010	4	1.30	4.19	1.16-1.36	0.83-1.40
S77	(0.40)	210 033	4	0.80	4.73	0.91-1.10	0.47-1.16	0.45-1.14
S79	0.74	499 221	3	0.60	1.60	0.65-1.18	0.30-1.21
S82	0.69	438 044	4	0.50	9.61	0.49-0.62	0.37-0.83	0.51-0.69
S85	(0.40)	414 053	3	5.70	25.77	5.51-5.79	4.78-6.19

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