A spatially resolved study of ionized regions in galaxies at different ...
A spatially resolved study of ionized regions in galaxies at different ...
A spatially resolved study of ionized regions in galaxies at different ...
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4.4. Discussion 141<br />
8.4<br />
A B C<br />
8.4<br />
A B C<br />
12 + log(O/H)<br />
8.2<br />
8.0<br />
7.8<br />
12 + log(O/H)<br />
8.2<br />
8.0<br />
7.8<br />
7.6<br />
O 23<br />
7.6<br />
S 23 /O 23<br />
8.4<br />
A B C<br />
8.4<br />
A B C<br />
12 + log(O/H)<br />
8.2<br />
8.0<br />
7.8<br />
12 + log(O/H)<br />
8.2<br />
8.0<br />
7.8<br />
7.6<br />
N2<br />
7.6<br />
Ar 3 /O 3<br />
8.4<br />
A B C<br />
8.4<br />
A B C<br />
12 + log(O/H)<br />
8.2<br />
8.0<br />
7.8<br />
12 + log(O/H)<br />
8.2<br />
8.0<br />
7.8<br />
7.6<br />
S 23<br />
7.6<br />
O3N2<br />
Figure 4.18: The oxygen abundances and their uncerta<strong>in</strong>ties for each observed knot <strong>of</strong> J1657, as<br />
derived us<strong>in</strong>g <strong>different</strong> empirical calibr<strong>at</strong>ors. From upper to lower panel: O 23 , N2, and S 23 , <strong>at</strong> left<br />
and S 23 /O 23 , Ar 3 O 3 and O3N2 <strong>at</strong> right. The dash-dotted l<strong>in</strong>e represent the abundances and their<br />
uncerta<strong>in</strong>ties as derived from the direct method.
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