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	Figure 1: Reflectance spectrum of 2003 UB313 obtained on 2005 October 20.03 UT, normalized at 0.6 m. The spectrum of Pluto (Grundy & Fink 1996) and the spectrum 2005 FY9 (Licandro et al. 2006), both shifted vertically, are plotted for comparison.
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In the text

Figure 2: Reflectance spectra of TNOs 2003 UB313, 2005 FY9, and Pluto shifted vertically, in the two wavelength regions of the most prominent CH4 ice absorption bands. Upper: (A) is the spectrum of 2003 UB313 and overplotted (dashed lines) is the spectrum of pure methane ice grains of 1.5 cm diameter; (B) is the spectrum of 2005 FY9 and overplotted (dashed lines) the spectrum of pure methane ice grains of 4.5 cm diameter; (C) is the spectrum of Pluto and overplotted (dashed lines) the spectrum of pure methane ice grains of 500 m diameter; vertical dashed lines indicate the central position of pure methane ice bands (Grundy et al. 2002). Lower: (A) same as in upper figure; (B) is the spectrum of 2005 FY9 and overplotted (dashed lines) the spectrum of pure methane ice grains of 2.5 cm diameter; (C) as in upper figure.

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In the text

	Figure 3: Reflectance spectrum of TNOs 2003 UB313 (solid line) and the spectrum of pure methane ice grains of 1.5 cm diameter shifted by 15  (dashed line).
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In the text