All Figures

$\begin{figure} \par\includegraphics[width=68mm,clip]{3001fig1.eps} % \par\end{figure}$ Figure 1: The galactic distribution of our sample including 1474 individual objects. There is a clustering of objects at $190^\circ <l<280^\circ$ , the almost reddening free (up to 500 pc from the Sun) third galactic quadrant.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=154mm,clip]{3001fig2.eps}\par\end{figure}$ Figure 2: The distribution of Johnson V and Strömgren (b-y)₀ of the sample divided into "normal'' type and "other'' (all objects included in Renson 1991, Table 3 and Sect. 3.2) stars.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=70mm]{3001fig3.eps}\par\end{figure}$ Figure 3: The mean values and the corresponding root mean square scatter for all normal type objects with $\Delta a$ measurements. The straight lines are the 3 $\sigma$ fits through the errors, whereas the asterisks denote the outliers of objects not included in the catalogue of Renson (1991) discussed in Sect. 3.2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=70mm]{3001fig4.eps}\par\end{figure}$ Figure 4: The detection probability of the different investigated groups as listed in Table 3.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=175mm]{3001fig5.eps}\end{figure}$ Figure 5: Comparison of the detection capability of the $\Delta a$ and Geneva $\Delta (V1 - G)$ , as well as Zindices for all groups discussed in this paper. No objects of the CP1 and $\lambda$ Bootis group are within the range of valid Z values, defined for stars hotter than A0. Because neither Z nor $\Delta (V1 - G)$ show significant deviating values for CP3 objects, both diagrams are identical, so we display only the $\Delta (V1 - G)$ versus $\Delta a$ diagram. Since Z is not affected by gravity, the plot for supergiants was omitted. Areas with the different patterns denote the regions where the respective indices are insensitive to peculiarity. The detailed statistics of these data are listed in Table 5.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=68mm,clip]{3001fig1.eps} % \par\end{figure}$	Figure 1: The galactic distribution of our sample including 1474 individual objects. There is a clustering of objects at $190^\circ <l<280^\circ$ , the almost reddening free (up to 500 pc from the Sun) third galactic quadrant.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=154mm,clip]{3001fig2.eps}\par\end{figure}$	Figure 2: The distribution of Johnson V and Strömgren (b-y)₀ of the sample divided into "normal'' type and "other'' (all objects included in Renson 1991, Table 3 and Sect. 3.2) stars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=70mm]{3001fig3.eps}\par\end{figure}$	Figure 3: The mean values and the corresponding root mean square scatter for all normal type objects with $\Delta a$ measurements. The straight lines are the 3 $\sigma$ fits through the errors, whereas the asterisks denote the outliers of objects not included in the catalogue of Renson (1991) discussed in Sect. 3.2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=70mm]{3001fig4.eps}\par\end{figure}$	Figure 4: The detection probability of the different investigated groups as listed in Table 3.
Open with DEXTER