Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{260fig1.ps} \end{figure}$ Figure 1: Visible spectra of 2000 GN171 obtained during part of its rotational period. All spectra have been normalized at 5500 Å and shifted by 0.8 for clarity. The first acquired spectrum is labelled A, the second B and so on till the sixth (F). The UT time at the beginning of each observation is also indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{260fig2.ps} \end{figure}$ Figure 2: Composite lightcurve of 2001 GN171 obtained by relative photometry. The error bars contain the photon noise. The zero phase is at JD 2 452 742.67. We place above the data the letters A-F indicating the corresponding spectrum (represented in Fig. 1) taken just after each photometric data set.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{260fig3.ps} \end{figure}$ Figure 3: Visible spectra of the three Centaurs observed. Spectra have been normalized at 5500 Å and shifted of 0.7 for clarity. The colors indices transformed in spectral reflectance are also shown on each spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=7.45cm,clip]{260fig4.ps} \end{figure}$ Figure 4: Visible spectra of the six TNOs. Spectra have been normalized at 5500 Å and shifted of 0.7 for clarity. The colors indices transformed in spectral reflectance are also shown on each spectrum. For 2000 GN171 we represented here the mean spectrum of the six different exposures available.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{260fig5.ps} \end{figure}$ Figure 5: Top: visible spectrum of 2003 AZ84 with superimposed the linear continuum computed with a linear least squares fit to the smoothed spectral data; bottom: spectrum of 2003 AZ84 with the continuum removed.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{260fig6.ps} \end{figure}$ Figure 6: Plot of the spectral slope versus the perihelion distance for all the centaurs and TNOs whose visible spectrum is available from the Large Program and in literature. The size of the points is proportional to the estimated diameter of the bodies. The smaller points represent the objects with estimated diameters less than 50 km, and their size progressively increases in steps of 50 km for the Centaurs and 100 km for the TNOs according to the values given in Table 5. The biggest points correspond to TNOs with an estimated diameter larger than 900 km.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{260fig7.ps} \end{figure}$ Figure 7: Distribution of the Centaurs as a function of the spectral slope. The sample includes 15 objects observed via visible spectroscopy from the ESO Large Program and in the literature.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{260fig8.ps} \end{figure}$ Figure 8: Distribution of the Plutinos ( left) and of the TNOs ( right) as a function of the spectral slope. The sample comprises 19 objects observed via visible spectroscopy from the ESO Large Program and in the literature.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{260fig1.ps} \end{figure}$	Figure 1: Visible spectra of 2000 GN171 obtained during part of its rotational period. All spectra have been normalized at 5500 Å and shifted by 0.8 for clarity. The first acquired spectrum is labelled A, the second B and so on till the sixth (F). The UT time at the beginning of each observation is also indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{260fig2.ps} \end{figure}$	Figure 2: Composite lightcurve of 2001 GN171 obtained by relative photometry. The error bars contain the photon noise. The zero phase is at JD 2 452 742.67. We place above the data the letters A-F indicating the corresponding spectrum (represented in Fig. 1) taken just after each photometric data set.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{260fig3.ps} \end{figure}$	Figure 3: Visible spectra of the three Centaurs observed. Spectra have been normalized at 5500 Å and shifted of 0.7 for clarity. The colors indices transformed in spectral reflectance are also shown on each spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.45cm,clip]{260fig4.ps} \end{figure}$	Figure 4: Visible spectra of the six TNOs. Spectra have been normalized at 5500 Å and shifted of 0.7 for clarity. The colors indices transformed in spectral reflectance are also shown on each spectrum. For 2000 GN171 we represented here the mean spectrum of the six different exposures available.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{260fig5.ps} \end{figure}$	Figure 5: Top: visible spectrum of 2003 AZ84 with superimposed the linear continuum computed with a linear least squares fit to the smoothed spectral data; bottom: spectrum of 2003 AZ84 with the continuum removed.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{260fig7.ps} \end{figure}$	Figure 7: Distribution of the Centaurs as a function of the spectral slope. The sample includes 15 objects observed via visible spectroscopy from the ESO Large Program and in the literature.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{260fig8.ps} \end{figure}$	Figure 8: Distribution of the Plutinos ( left) and of the TNOs ( right) as a function of the spectral slope. The sample comprises 19 objects observed via visible spectroscopy from the ESO Large Program and in the literature.
Open with DEXTER