All Figures

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{9467fig1.ps}\end{figure}$ Figure 1: Comparison between spectrophotometry from Clampitt & Burstein (1997) and normalised fluxes at 5560 Å with the fundamental parameters adopted for the abundance analysis of the star HD 73345.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{9467fig2.ps}\end{figure}$ Figure 2: Comparison between the abundances derived for HD 73045 ( $\ensuremath{{\upsilon}\sin i}$ = 10 ${\rm km~s}^{-1}$ - open circles in the upper panel) and HD 73746 ( $\ensuremath{{\upsilon}\sin i}$ = 95 ${\rm km~s}^{-1}$ - open circles in the lower panel) adopting a proper line selection and the lines used to determine the abundances of HD 72757 ( $\ensuremath{{\upsilon}\sin i}$ = 179 ${\rm km~s}^{-1}$ - open squares in both panels).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9467fig3.ps}\end{figure}$ Figure 3: The upper panels show the variation of the standard deviation from the mean abundance of Fe, Ni, Cr and Ti as a function of $\upsilon _{{\rm mic}}$ , for HD 73730 ( $\ensuremath{{\upsilon}\sin i}$ = 29 ${\rm km~s}^{-1}$ ) and HD 73746 ( $\ensuremath{{\upsilon}\sin i}$ = 95 ${\rm km~s}^{-1}$ ). The lower panels show the variation of the mean abundance as a function of $\upsilon _{{\rm mic}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9467fig4.ps}\end{figure}$ Figure 4: As for Fig. 3, but for HD 72757 ( $\ensuremath{{\upsilon}\sin i}$ = 179 ${\rm km~s}^{-1}$ ) and HD 73798 ( $\ensuremath{{\upsilon}\sin i}$ = 200 ${\rm km~s}^{-1}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9467fig5.ps}\end{figure}$ Figure 5: Comparison between the mean abundances obtained for Am, A- and F-type stars indicated by an open circle, square and triangle respectively. The error bars are the standard deviations from the calculated mean abundances. In the case of only one measurement, no error bar is shown. A- and F-type stars show a similar abundance pattern. The Am stars show the typical peculiar abundance pattern described in detail in Paper I.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9467fig6.ps}\end{figure}$ Figure 6: Hertzsprung-Russell diagram of the Praesepe cluster. The crosses and filled squares show the position on the HR diagram for the Am and normal A- and F-type stars, respectively. The open squares indicate the spectroscopic binaries. We did not correct the luminosity of these stars due to the presence of a companion, but we assume it less than 0.1 dex. The error bar in luminosity is 0.07 dex. The dashed line shows an isochrone from Girardi et al. (2002) for the age and metallicity given in the literature ( $\ensuremath{\log t}$ = 8.85 dex; Z = 0.024 dex). The solid line shows the isochrone corresponding to our best fit ( $\ensuremath{\log t}$ = 8.77 dex; Z = 0.030 dex).
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In the text

$\begin{figure} \par\includegraphics[width=9.6cm,clip]{9467fig7.ps}\end{figure}$ Figure 7: Abundances relative to the Sun (Asplund et al. 2005) of C, O, Ca and Sc as a function of $T_{{\rm eff}}$ and $\ensuremath{{\upsilon}\sin i}$ for normal A-type stars (circle), Am stars (square) and normal F-type stars (triangle). A correlation between abundances of C, O, Ca and $\ensuremath{{\upsilon}\sin i}$ is found for Am stars; an anticorrelation between Sc abundance and $\ensuremath{{\upsilon}\sin i}$ is found for Am stars.
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In the text

$\begin{figure} \par\includegraphics[width=9.6cm,clip]{9467fig8.ps}\end{figure}$ Figure 8: Same as in Fig. 7 but for Na, Mg, Si and S. No correlation is found.
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In the text

$\begin{figure} \par\includegraphics[width=9.6cm,clip]{9467fig9.ps}\end{figure}$ Figure 9: Same as in Fig. 7 but for Ti, Cr, Fe, Ni, Y and Ba. No correlation is found for Ti. An anticorrelation between Cr, Fe, Ni, Y and Ba abundance and $\ensuremath{{\upsilon}\sin i}$ is found for Am stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9467fig10.ps}\end{figure}$ Figure 10: Abundances relative to the Sun (Asplund et al. 2005) of Mg, Ca and Fe as a function of the $M/M\odot$ . No correlations are found.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{9467fig11.ps}\end{figure}$ Figure 11: Abundances relative to the Sun (Asplund et al. 2005) of C, O, Na, Mg, S and Si as a function of the Fe abundance.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{9467fig12.ps}\end{figure}$ Figure 12: Same as in Fig. 11 but for Ca, Sc, Ti, Cr, Mn, Ni, Y and Ba.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9467fig13.ps}\end{figure}$ Figure 13: Comparison between the spectra of HD 73666 obtained with the ESPaDOnS spectropolarimeter (blue line) and the SOPHIE spectrograph (red line) in the region of the He I multiplet at $\sim$ 4471.5 Å. No difference is visible between the two spectra, apart the one due to the different spectral resolution of the two instruments.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9467fig14.ps}\end{figure}$ Figure 14: Same as for Fig. 13, but in the region of the strong Fe II line at 5018.440 Å.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9467fig15.ps}\end{figure}$ Figure 15: Comparison between the mean abundance of the Am stars analysed in Paper I and the Am star HD 74656. This plot confirms the Am classification of this star.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{9467fig16.ps}\end{figure}$ Figure 16: Portion of the spectrum of HD 72757 ( $\ensuremath{{\upsilon}\sin i}$ = 179 ${\rm km~s}^{-1}$ ) and the synthetic spectrum after the complete abundance analysis in black and red respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{9467fig1.ps}\end{figure}$	Figure 1: Comparison between spectrophotometry from Clampitt & Burstein (1997) and normalised fluxes at 5560 Å with the fundamental parameters adopted for the abundance analysis of the star HD 73345.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9467fig4.ps}\end{figure}$	Figure 4: As for Fig. 3, but for HD 72757 ( $\ensuremath{{\upsilon}\sin i}$ = 179 ${\rm km~s}^{-1}$ ) and HD 73798 ( $\ensuremath{{\upsilon}\sin i}$ = 200 ${\rm km~s}^{-1}$ ).
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$\begin{figure} \par\includegraphics[width=9.6cm,clip]{9467fig8.ps}\end{figure}$	Figure 8: Same as in Fig. 7 but for Na, Mg, Si and S. No correlation is found.
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$\begin{figure} \par\includegraphics[width=9.6cm,clip]{9467fig9.ps}\end{figure}$	Figure 9: Same as in Fig. 7 but for Ti, Cr, Fe, Ni, Y and Ba. No correlation is found for Ti. An anticorrelation between Cr, Fe, Ni, Y and Ba abundance and $\ensuremath{{\upsilon}\sin i}$ is found for Am stars.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9467fig10.ps}\end{figure}$	Figure 10: Abundances relative to the Sun (Asplund et al. 2005) of Mg, Ca and Fe as a function of the $M/M\odot$ . No correlations are found.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{9467fig11.ps}\end{figure}$	Figure 11: Abundances relative to the Sun (Asplund et al. 2005) of C, O, Na, Mg, S and Si as a function of the Fe abundance.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{9467fig12.ps}\end{figure}$	Figure 12: Same as in Fig. 11 but for Ca, Sc, Ti, Cr, Mn, Ni, Y and Ba.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9467fig13.ps}\end{figure}$	Figure 13: Comparison between the spectra of HD 73666 obtained with the ESPaDOnS spectropolarimeter (blue line) and the SOPHIE spectrograph (red line) in the region of the He I multiplet at $\sim$ 4471.5 Å. No difference is visible between the two spectra, apart the one due to the different spectral resolution of the two instruments.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9467fig14.ps}\end{figure}$	Figure 14: Same as for Fig. 13, but in the region of the strong Fe II line at 5018.440 Å.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9467fig15.ps}\end{figure}$	Figure 15: Comparison between the mean abundance of the Am stars analysed in Paper I and the Am star HD 74656. This plot confirms the Am classification of this star.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{9467fig16.ps}\end{figure}$	Figure 16: Portion of the spectrum of HD 72757 ( $\ensuremath{{\upsilon}\sin i}$ = 179 ${\rm km~s}^{-1}$ ) and the synthetic spectrum after the complete abundance analysis in black and red respectively.
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