Table 3: Results of the spectral synthesis analysis of the Lyman-break galaxies. Objects are identified by numbers adopted in this work, by Papovich and by Williams (first three columns). For each source the table reports redshift, total number of models analyzed, effective number of SSPs involved in the best fit, stellar mass and $\chi ^2$ of best fit and 2 $\sigma$ mass range due to degeneracies. Last column summarizes the results of our simulated SIRTF/IRAC observations of ly-break sources: IRAC will sample the restframe near-IR light at $z\sim 2{-}3$ , therefore significantly reducing the uncertainty on the stellar mass estimate (see text for details).
Obj ID Pap. ID Will. z $N_{\rm tot}$ $N_{\rm SSP}$ $\chi^2_{\rm opt}$ Mass (b.f.) $\Delta M$ $\Delta M_{\rm SIRTF}$

# (1) (2) (3) mdls. b.f. b.f. $[10^{11}~M_\odot]$ $[10^{11}~M_\odot]$ $[10^{11}~M_\odot]$

Ly1 110 2-449.0 2.005 230403 3 5.13 0.21 0.16-2.47 0.27-0.55

Ly2 503 2-903.0 2.233 195602 3 4.24 0.13 0.04-0.24 0.09-0.19

Ly3 67 2-82.1 2.267 195587 3 1.47 0.04 0.03-0.84 0.04-0.09

Ly4 804 4-639.0 2.591 212778 2 10.99 0.09 0.03-0.28 0.03-0.09

Ly5 1352 4-497.0 2.800 199203 3 5.87 0.02 0.02-0.29 0.02-0.06

Ly6 1541 4-363.0 2.980 217529 3 9.02 0.18 0.05-0.35 0.06-0.20

Ly7 661 2-643.0 2.991 264435 2 7.54 0.04 0.02-0.13 0.03-0.06

Ly8 273 2-76.11 3.160 278399 2 2.29 0.56 0.27-1.35 0.38-0.81

(1): ID number in Papovich et al. (2001);

(2): ID number in Williams et al. (1996);

(3): Spectroscopic redshifts by Steidel et al. (1996) and Lowental et al. (1997).

**Table 3:** Results of the spectral synthesis analysis of the Lyman-break galaxies. Objects are identified by numbers adopted in this work, by Papovich and by Williams (first three columns). For each source the table reports redshift, total number of models analyzed, effective number of SSPs involved in the best fit, stellar mass and $\chi ^2$ of best fit and 2 $\sigma$ mass range due to degeneracies. Last column summarizes the results of our simulated SIRTF/IRAC observations of ly-break sources: IRAC will sample the restframe near-IR light at $z\sim 2{-}3$ , therefore significantly reducing the uncertainty on the stellar mass estimate (see text for details).
Obj	ID Pap.	ID Will.	z	$N_{\rm tot}$	$N_{\rm SSP}$	$\chi^2_{\rm opt}$	Mass (b.f.)	$\Delta M$	$\Delta M_{\rm SIRTF}$
#	(1)	(2)	(3)	mdls.	b.f.	b.f.	$[10^{11}~M_\odot]$	$[10^{11}~M_\odot]$	$[10^{11}~M_\odot]$
Ly1	110	2-449.0	2.005	230403	3	5.13	0.21	0.16-2.47	0.27-0.55
Ly2	503	2-903.0	2.233	195602	3	4.24	0.13	0.04-0.24	0.09-0.19
Ly3	67	2-82.1	2.267	195587	3	1.47	0.04	0.03-0.84	0.04-0.09
Ly4	804	4-639.0	2.591	212778	2	10.99	0.09	0.03-0.28	0.03-0.09
Ly5	1352	4-497.0	2.800	199203	3	5.87	0.02	0.02-0.29	0.02-0.06
Ly6	1541	4-363.0	2.980	217529	3	9.02	0.18	0.05-0.35	0.06-0.20
Ly7	661	2-643.0	2.991	264435	2	7.54	0.04	0.02-0.13	0.03-0.06
Ly8	273	2-76.11	3.160	278399	2	2.29	0.56	0.27-1.35	0.38-0.81

Source LaTeX | All tables | In the text

(1): ID number in Papovich et al. (2001);
(2): ID number in Williams et al. (1996);
(3): Spectroscopic redshifts by Steidel et al. (1996) and Lowental et al. (1997).