1.18 & $2\times60$\
2001 Dec. 16 & 13 & EMMI & 3980–9400 & 9 & 1.64 & $3\times60$\
2001 Dec. 23 & 20 & LRIS & 3400–10300 & 7 & 2.49 & 60\
2002 Jan. 13 & 41 & EFOSC2 & 3360–10300 & 9 & 1.87 & $3\times90$\
2002 Jan. 17 & 45 & LRIS & 3520–10000 & 7 & 4.09 & 360\
2002 Jan. 18 & 46 & LRIS & 3500–5380 & 3 & 4.99 & 450\
2002 Jan. 18 & 46 & LRIS & 5710–7000 & 2 & 4.99 & 450\
2002 Jan. 29 & 57 & LDSS2 & 3600–10000 & 13 & 2.61 & 90\
2002 Aug. 16 & 256 & FORS1 & 4000–8600 & 12 & 1.04 & $4\times1200$\
2002 Oct. 8 & 309 & LRIS & 3150–9420 & 6 & 2.18 & $2\times600$\
2002 Nov. 8 & 340 & LRIS & 3100–9410 & 6 & 2.05 & 900\

All spectra were reduced using standard techniques [e.g., @Foley03]. Standard CCD processing and spectrum extraction for the LRIS data were completed with IRAF[^1], and the data were extracted with the optimal algorithm of @Horne86. We obtained the wavelength scale from low-order polynomial fits to calibration-lamp spectra. Small 