Table 1: Log of VLT spectroscopic observations.
GRB UT date^a $\Delta T$ instr. grism (filter) coverage^b slit width resolution^c dispersion exptime seeing airmass

(days) (Å) ( $^{\prime \prime }$ ) (Å) (Å/pixel) (min) ( $^{\prime \prime }$ )

991216 1999 Dec. 18.159 1.49 FORS1 150I (OG590) 3800-9500 1 24 5.3 $6\times10^{{d}}$ 0.6 1.24-1.27

011211 2001 Dec. 13.253 1.45 FORS2 300V 3600-8900 1 10 2.6 $9\times10$ 1.1 1.20-1.94

021211 2002 Dec. 30.294 18.82 FORS2 300V 3600-9500 1 11 3.2 $3\times10$ 0.7 1.20-1.24

^a
Start of the first exposure.
^b
Without order sorting filter, the second order will start to contaminate the spectrum above $\sim$ 7000 Å.
^c
The resolution is approximately constant across the entire spectrum.
^d
The first three exposures are taken without order sorting filter, followed by three with filter.

**Table 1:** Log of VLT spectroscopic observations.
GRB	UT date^a	$\Delta T$	instr.	grism (filter)	coverage^b	slit width	resolution^c	dispersion	exptime	seeing	airmass
		(days)			(Å)	( $^{\prime \prime }$ )	(Å)	(Å/pixel)	(min)	( $^{\prime \prime }$ )
991216	1999 Dec. 18.159	1.49	FORS1	150I (OG590)	3800-9500	1	24	5.3	$6\times10^{{d}}$	0.6	1.24-1.27
011211	2001 Dec. 13.253	1.45	FORS2	300V	3600-8900	1	10	2.6	$9\times10$	1.1	1.20-1.94
021211	2002 Dec. 30.294	18.82	FORS2	300V	3600-9500	1	11	3.2	$3\times10$	0.7	1.20-1.24

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