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$\begin{figure} \includegraphics[width=18cm]{Barucci_Fig1.ps} \end{figure}$ Figure 1: Individual emissivity spectra of 21 Lutetia acquired on 10 December 2005 from 17:32 UT to 11 December 2006 02:27 UT (the UT time corresponds to the start of the exposure).
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In the text

$\begin{figure} \includegraphics[width=18cm]{Barucci_Fig2.ps} \end{figure}$ Figure 2: Individual emissivity spectra of 2867 Steins acquired on 22 November 2005 from 06:23 to 13:11, UT time (the UT time corresponds to the start of the exposure).
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In the text

$\begin{figure} \includegraphics[width=9cm]{Barucci_Fig3.ps} \end{figure}$ Figure 3: The emissivity of Lutetia (average of the 14 individual spectra) compared with the emissivity of the Allende meteorite (from the ASTER database, with particle size 0-75 $\mu$ m) and of the Odessa meteorite (from the RELAB database, with particle size 45-90 $\mu$ m). The error bars of the emissivity spectrum of Lutetia are $\sim$ 5% considering errors due both to the thermal data and to the model incertitude. The Christiansen, Reststrahlen and Transparency features are indicated as C, R, and T.
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In the text

$\begin{figure} \includegraphics[width=9cm]{Barucci_Fig4.ps} \end{figure}$ Figure 4: The emissivity of Lutetia (average of the 14 individual spectra) compared with the emissivity of the Ornans meteorite by Barucci et al. (2005) at different grain dimensions (0-20 $\mu$ m, continuous line; 20-50 $\mu$ m, dotted line; 50-100 $\mu$ m, dashed line; and >100 $\mu$ m , dashed-dotted line), and the emissivity of the Vigarano meteorite obtained with new laboratory experiments at different grain dimensions. Vigarano (1): continuous line for 0-20 $\mu$ m; dotted line for 20-50 $\mu$ m, and dashed line for 50-100 $\mu$ m; Vigarano (2): continuous line for 100-150 $\mu$ m, and dashed line for grain size >150 $\mu$ m. All the spectra are shifted for clarity. The Christiansen, Reststrahlen, and Transparency features are indicated as C, R, and T.
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In the text

$\begin{figure} \includegraphics[width=9cm,angle=0]{Barucci_Fig5.ps} \end{figure}$ Figure 5: The emissivity of Steins (average of the 14 individual spectra) compared with the emissivity of the aubrite meteorite ALH84007 taken from the ASTER database and that of the enstatite sample (with particle size 0-50 $\mu$ m) taken from Barucci et al. (2005). All the spectra are shifted for clarity. The Christiansen, Reststrahlen, and Transparency features are indicated as C, R, and T. The error bars of the emissivity spectrum of Steins are $\sim$ 11% considering both the errors due to the thermal data and to the model incertitude.
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In the text

$\begin{figure} \includegraphics[width=18cm]{Barucci_Fig1.ps} \end{figure}$	Figure 1: Individual emissivity spectra of 21 Lutetia acquired on 10 December 2005 from 17:32 UT to 11 December 2006 02:27 UT (the UT time corresponds to the start of the exposure).
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$\begin{figure} \includegraphics[width=18cm]{Barucci_Fig2.ps} \end{figure}$	Figure 2: Individual emissivity spectra of 2867 Steins acquired on 22 November 2005 from 06:23 to 13:11, UT time (the UT time corresponds to the start of the exposure).
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