All Figures

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f1.ps}\end{figure}$ Figure 1: Absolute magnitudes H_v of Chiron as a function of heliocentric distance and time.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f2.ps}\end{figure}$ Figure 2: The amplitude of the lightcurve $\Delta m_{v}$ of Chiron as a function of the absolute magnitude H_v. The data points are the observations reported in Table 1 (except those of 29 February 1988 and 20 February 1993).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f3.ps}\end{figure}$ Figure 3: Equatorial temperature profiles over the nucleus surface for thermal inertia I=0, 10, 100 J K^-1 m^-2 s^-1/2 and $\infty$ at r=8.5 AU.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3595_f4.ps}\end{figure}$ Figure 4: Value of the $\chi ^2$ expression as a function of the radius $r_{\rm n}$ and the thermal inertia I. The cross represents best estimate of $r_{\rm n}$ and I, i.e. where $\chi ^2$ is minimum.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f5.ps}\end{figure}$ Figure 5: The SED of the nucleus of Chiron for the mixed model (MM) with a radius $r_{\rm n}=71\pm 5$ km and a thermal inertia I=3⁺⁵_-3 MKS. The squares are the ISOPHOT data at 25, 60, 100 and 160 $\mu$ m with their $1\sigma$ error bars.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3595_f6.ps}\end{figure}$ Figure 6: The albedo-radius diagram for Chiron. The infrared constraints come from the ISOPHOT observations with the models presented in Fig. 3. The visible constraint is given by the visible absolute magnitude of the nucleus of Chiron $H_0=7.28\pm 0.08$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f7.ps}\end{figure}$ Figure 7: Observed spectra of Chiron compared to laboratory experiments with mixtures of charcoal and water ice.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f8.ps}\end{figure}$ Figure 8: Observed spectra of Chiron compared to two mixtures of astronomical silicate and water ice grains in different proportions. The grain size is 10 $\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f9.ps}\end{figure}$ Figure 9: Observed spectra of Chiron compared to two mixtures of astronomical silicate and water ice grains, with grain sizes of 1 and 100 $\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f10.ps}\end{figure}$ Figure 10: Observed spectra of Chiron compared to three different mixtures of 30% of water ice +70% of refractory grains (silicate, glassy carbon or kerogen). The grain size is 10 $\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f11.ps}\end{figure}$ Figure 11: Determination of the radius of Chiron from the infrared and radio observations of Table 2, using a mixed model (MM) with a geometric albedo of 0.11 and a thermal inertia of 3 MKS. The solid bold line and the hatched band represent our determination of $71\pm 5$ km.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f12.ps}\end{figure}$ Figure 12: Determination of the radius of Chariklo from the 20.3 $\mu$ m infrared and 1.2 mm radio observations of Table 7. Differents symbols are used for I=0, 10 and 100 MKS. The symbols at 1.2 mm have been deliberately offset left-right for clarity. The solid bold line and the hatched band represent our determination of $118\pm 6$ km.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f13.ps}\end{figure}$ Figure 13: The observed spectrum of Chariklo compared to four different mixtures of water ice and refractory grains (silicate, glassy carbon or kerogen). The grain size is 10 $\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f1.ps}\end{figure}$	Figure 1: Absolute magnitudes H_v of Chiron as a function of heliocentric distance and time.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f2.ps}\end{figure}$	Figure 2: The amplitude of the lightcurve $\Delta m_{v}$ of Chiron as a function of the absolute magnitude H_v. The data points are the observations reported in Table 1 (except those of 29 February 1988 and 20 February 1993).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f3.ps}\end{figure}$	Figure 3: Equatorial temperature profiles over the nucleus surface for thermal inertia I=0, 10, 100 J K^-1 m^-2 s^-1/2 and $\infty$ at r=8.5 AU.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3595_f4.ps}\end{figure}$	Figure 4: Value of the $\chi ^2$ expression as a function of the radius $r_{\rm n}$ and the thermal inertia I. The cross represents best estimate of $r_{\rm n}$ and I, i.e. where $\chi ^2$ is minimum.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f5.ps}\end{figure}$	Figure 5: The SED of the nucleus of Chiron for the mixed model (MM) with a radius $r_{\rm n}=71\pm 5$ km and a thermal inertia I=3⁺⁵_-3 MKS. The squares are the ISOPHOT data at 25, 60, 100 and 160 $\mu$ m with their $1\sigma$ error bars.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3595_f6.ps}\end{figure}$	Figure 6: The albedo-radius diagram for Chiron. The infrared constraints come from the ISOPHOT observations with the models presented in Fig. 3. The visible constraint is given by the visible absolute magnitude of the nucleus of Chiron $H_0=7.28\pm 0.08$ .
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f7.ps}\end{figure}$	Figure 7: Observed spectra of Chiron compared to laboratory experiments with mixtures of charcoal and water ice.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f8.ps}\end{figure}$	Figure 8: Observed spectra of Chiron compared to two mixtures of astronomical silicate and water ice grains in different proportions. The grain size is 10 $\mu$ m.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f9.ps}\end{figure}$	Figure 9: Observed spectra of Chiron compared to two mixtures of astronomical silicate and water ice grains, with grain sizes of 1 and 100 $\mu$ m.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f10.ps}\end{figure}$	Figure 10: Observed spectra of Chiron compared to three different mixtures of 30% of water ice +70% of refractory grains (silicate, glassy carbon or kerogen). The grain size is 10 $\mu$ m.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f11.ps}\end{figure}$	Figure 11: Determination of the radius of Chiron from the infrared and radio observations of Table 2, using a mixed model (MM) with a geometric albedo of 0.11 and a thermal inertia of 3 MKS. The solid bold line and the hatched band represent our determination of $71\pm 5$ km.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3595_f12.ps}\end{figure}$	Figure 12: Determination of the radius of Chariklo from the 20.3 $\mu$ m infrared and 1.2 mm radio observations of Table 7. Differents symbols are used for I=0, 10 and 100 MKS. The symbols at 1.2 mm have been deliberately offset left-right for clarity. The solid bold line and the hatched band represent our determination of $118\pm 6$ km.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3595_f13.ps}\end{figure}$	Figure 13: The observed spectrum of Chariklo compared to four different mixtures of water ice and refractory grains (silicate, glassy carbon or kerogen). The grain size is 10 $\mu$ m.
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