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Figure 1:
[OIII]5007 line maps ( left) and near-IR spectra
( right)
of the galaxies in the AMAZE sample presented here. Each [OIII]5007 map has a size of
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Figure 2: Same as Fig. 1 for four additional sources. |
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Figure 3: Same as Figs. 1, 2 for one additional source. |
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Figure 4: Composite spectrum of the nine sources presented in this paper. |
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Figure 5:
Relations between strong emission line ratios and gas metallicity. Blue squares are
low metallicity galaxies (from Nagao et al. 2006) for which the metallicity is inferred through
the electron temperature ![]() |
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Figure 6:
Example of the diagnostic tools used to determine the metallicity
in the specific case of the composite spectrum. The upper left panel shows the
best solution (blue cross) and the 1![]() ![]() ![]() |
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Figure 7:
Mass-metallicity relation observed at different redshifts.
The blue, solid and dotted lines indicate the
mass-metallicity relation and its dispersion observed at
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Figure 8: Comparison of the mass-metallicity relation observed at different redshifts, as parametrized by the analytical function Eq. (2) and coefficients in Table 5. |
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Figure 9:
Average metallicity of star forming galaxies as a function of the cosmic age
of the Universe, relative to local galaxies,
for three different families of galaxies with different stellar masses
(
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Figure 10:
Comparison between models/simulations predictions for the mass-metallicity relation at
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Figure 11:
Evolutionary tracks of individual galaxies on the
mass-metallicity diagram according to some
models for the formation of spheroids presented in Granato et al. (2004) (green solid lines)
and in Pipino et al. (2006) (violet dashed lines),
compared with the mass-metallicity relation observed
at ![]() |
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