All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5518fg1a.ps}\includegraphics{5518fg1b.ps}} \end{figure}$ Figure 1: Applying the Fourier technique. On the left (126) Velleda and on the right (854) Frostia, examples of the technique in a high and medium signal-to-noise spectra.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{5518fg2a.ps}} \end{figure}$ Figure 2: Proper element distribution of asteroids in the inner belt region: a) semi-major axis versus eccentricity and b) semi-major axis versus sine of inclination.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[angle=270]{5518fg3a.ps}} \end{figure}$ Figure 3: Proper element distribution of the classified asteroids: a) semi-major axis versus eccentricity and b) semi-major axis versus sine of inclination space. The red (open) and blue (filled) points represent asteroids with featured and featureless spectra, respectively.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=270,width=\textwi... ...x{8.8cm}{!}{\includegraphics[angle=270,width=\textwidth]{5518fg4c}} \end{figure}$ Figure 4: Number distribution of classified asteroids: left, semi-major axis versus eccentricity and right, semi-major axis versus sine of inclination. The top and bottom panels represent asteroids with featureless and featured spectra, respectively. The gray scale code used is given below the figure.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=270,width=\textwi... ....8cm}{!}{\includegraphics[angle=270,width=\textwidth]{5518fg5d.ps}} \end{figure}$ Figure 5: Number distribution of asteroids with featureless spectra: left, semi-major axis versus eccentricity and right, semi-major axis versus sine of inclination. The upper, middle and lower panels represent asteroids of the C-, X- and D-groups as defined in the text, respectively. The gray scale code used is given below the figure.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=270,width=\textwi... ....8cm}{!}{\includegraphics[angle=270,width=\textwidth]{5518fg6d.ps}} \end{figure}$ Figure 6: Number distribution of asteroids with featured spectra: left, semi-major axis versus eccentricity and right, semi-major axis versus sine of inclination. The upper, middle and lower panels represent asteroids of the S-, AR- and V-group as defined in the text, respectively. The gray scale used code is given below the figure.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[width=\textwidth]{5518fg7a.ps}} \end{figure}$ Figure 7: De-biased populations of the inner Main Belt. Featured, dashed line, and featureless, continuous line.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm]{5518fg8a.eps}\includegraphics[width=8.3cm]{5518fg8b.eps} \end{figure}$ Figure 8: Dynamical maps of the inner region of the asteroidal belt on the (a,e)-plane ( left) and (a, I)-plane ( right) of the osculating elements (the initial inclination on the left panel and initial eccentricity on the right panel were fixed at the current values of those of Vesta). The domains of chaotic motion (the vertical dark strips) are associated with two- and three-body mean-motion resonances and are labeled on the top of the panels by numbers from 1 to 9 (see Table 3). For reference we also show the location in the proper elements space of Vesta family members, in cyan, Massalia, in blue, Nysa, in yellow, Erigone, in magenta, and Baptistina, in green.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[width=\textwidth]{5518fg9a.eps}} \end{figure}$ Figure 9: Location of the nonlinear secular resonances in the inner Main Belt computed for the inclination of (4) Vesta ( $i=6\hbox{$.\!\!^\circ$ }4$ ). The resonances involving perihelia are shown in blue, in green those of nodes and in magenta those of both perihelia and nodes. Vesta family members (in the proper elements space) are shown by cyan dots and the 31 V-type objects currently outside the family by red circles.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[width=\textwidth]{5518fg10.ps}} \end{figure}$ Figure 10: Filtered spectra of the observed asteroids.
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In the text

$\begin{figure}\par\resizebox{18cm}{!}{\includegraphics[width=\textwidth]{5518fg11.ps}} \end{figure}$ Figure 10: continued.
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In the text

$\begin{figure}\par\resizebox{18cm}{!}{\includegraphics[width=\textwidth]{5518fg12.ps}} \end{figure}$ Figure 10: continued.
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In the text

$\begin{figure}\par\resizebox{18cm}{!}{\includegraphics[width=\textwidth]{5518fg13.ps}} \end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{5518fg1a.ps}\includegraphics{5518fg1b.ps}} \end{figure}$	Figure 1: Applying the Fourier technique. On the left (126) Velleda and on the right (854) Frostia, examples of the technique in a high and medium signal-to-noise spectra.
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=270]{5518fg2a.ps}} \end{figure}$	Figure 2: Proper element distribution of asteroids in the inner belt region: a) semi-major axis versus eccentricity and b) semi-major axis versus sine of inclination.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[angle=270]{5518fg3a.ps}} \end{figure}$	Figure 3: Proper element distribution of the classified asteroids: a) semi-major axis versus eccentricity and b) semi-major axis versus sine of inclination space. The red (open) and blue (filled) points represent asteroids with featured and featureless spectra, respectively.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=270,width=\textwi... ...x{8.8cm}{!}{\includegraphics[angle=270,width=\textwidth]{5518fg4c}} \end{figure}$	Figure 4: Number distribution of classified asteroids: left, semi-major axis versus eccentricity and right, semi-major axis versus sine of inclination. The top and bottom panels represent asteroids with featureless and featured spectra, respectively. The gray scale code used is given below the figure.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=270,width=\textwi... ....8cm}{!}{\includegraphics[angle=270,width=\textwidth]{5518fg5d.ps}} \end{figure}$	Figure 5: Number distribution of asteroids with featureless spectra: left, semi-major axis versus eccentricity and right, semi-major axis versus sine of inclination. The upper, middle and lower panels represent asteroids of the C-, X- and D-groups as defined in the text, respectively. The gray scale code used is given below the figure.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=270,width=\textwi... ....8cm}{!}{\includegraphics[angle=270,width=\textwidth]{5518fg6d.ps}} \end{figure}$	Figure 6: Number distribution of asteroids with featured spectra: left, semi-major axis versus eccentricity and right, semi-major axis versus sine of inclination. The upper, middle and lower panels represent asteroids of the S-, AR- and V-group as defined in the text, respectively. The gray scale used code is given below the figure.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[width=\textwidth]{5518fg7a.ps}} \end{figure}$	Figure 7: De-biased populations of the inner Main Belt. Featured, dashed line, and featureless, continuous line.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[width=\textwidth]{5518fg10.ps}} \end{figure}$	Figure 10: Filtered spectra of the observed asteroids.
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$\begin{figure}\par\resizebox{18cm}{!}{\includegraphics[width=\textwidth]{5518fg11.ps}} \end{figure}$	Figure 10: continued.
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