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
and mass of the best fit
solution. The last three columns report three different estimates of
the mass uncertainties due to degeneracies:
at 68.3% and 95.5%
confidence levels (corresponding to 1
and 2
)
and 2
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
for the analytic SFH method (see text for details),
mass of the best fit solution and 2
(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
yrs old) with solar metallicity, c) two old
populations (
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
of best fit and 2
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
,
therefore significantly reducing the uncertainty on the
stellar mass estimate (see text for details).