All Figures

Figure 1: Light curve of the afterglow of GRB 021211. Filled circles represent data from published or submitted works (Fox et al. 2003; Li et al. 2003; Pandey et al. 2003), open circles are converted from HST measurements (Fruchter et al. 2002), while filled diamonds indicate our data; the arrow shows the epoch of our spectroscopic measurement. The dotted and dot-dashed lines represent the afterglow (see text) and host contribution respectively. The dashed line shows the light curve of SN 1994I reported at z = 1.006 and dereddened with AV = 2 (from Lee et al. 1995). The solid line shows the sum of the three contributions.

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In the text

	Figure 2: Rest-frame spectrum of the afterglow of GRB 021211 on 2003 Jan. 8.27 UT, or 27 days after the GRB (thick lines), compared with that of several SNe (thin lines).
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In the text

	Figure 3: Comparison of the spectrum of the GRB bump to the ones of SN 1994I taken at different times. Each plot has a different AV, in order to better match our spectrum (we adopted the extinction law by Cardelli et al. 1989). For reference, SN 1994I reached its B-band maximum on 1994 Apr. 9.
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In the text