![\begin{figure}
\par\includegraphics[width=7.7cm,clip]{9969fig1.ps}\hspace*{3mm}
\includegraphics[width=7.7cm,clip]{9969fig2.ps}
\end{figure}](/articles/aa/full/2008/37/aa09969-08/img103.gif) |
Figure 1: Comparisons between iron line EW measurements of stars with different abundances and with similar (spectroscopic) temperatures. Two Praesepe stars are compared respectively with a star in IC 4651 (KW 326 versus AMC 4220, left panel) and in M 67 (KW 100 versus Sanders 1092, right panel). Fe I and Fe II lines are plotted with different symbols. KW 100 and Sanders 1092 have virtually the same temperature. AMC 4220 is evaluated to be about 100 K hotter than KW 326, which reduces the effect of the metallicity difference on the EW ratios between the two stars. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=7cm,clip]{9969fig3.ps}
\end{figure}](/articles/aa/full/2008/37/aa09969-08/img123.gif) |
Figure 2:
Abundance gradient as resulting from high-spectroscopy open
cluster chemical analyses. Data plotted and relative error bars are as
in Table 9; for Hyades only, we have adopted in this
figure a different value, i.e.
 dex, which takes into account
also other estimations of about 0.2 dex. The y-axis of the filled
symbol points refer to our datapoints. The line represents the -0.06 dex/kpc relation. |
| Open with DEXTER | |
In the text