All Tables

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).
Table 2: Results of the stellar-mass estimate for the ellipticals sample, based of SEDs fitting with solar metallicity SSPs. For each elliptical source in the HDFS (Rodighiero et al. 2001), spectroscopic (Vanzella et al. 2003; Sawicky & Mallen-Ornelas 2003) or photometric (if within parenthesis, Rodighiero) redshifts, total number of models produced by the spectrophotometric synthesis code, best fit parameters and $\chi ^2$ for the analytic SFH method (see text for details), mass of the best fit solution and 2 $\sigma$ (95.5% confidence) mass range due to degeneracies are reported. Third column reports a flag identifying red and blue sources. The SEDs of the red sources have been fitted with three different methods: a) analytic SFH, b) two simple stellar populations (10⁹ and $1.2 \times 10^{10}$ yrs old) with solar metallicity, c) two old populations ( $1.2 \times 10^{10}$ yrs) with different metallicities (Z=0.02, 0.008) - see also text and Fig. 3. The mass ranges reported for these objects include the results of all three fitting tecniques; on blue sources only the analytic SFH leads to good results.
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).