fields we determined the limits of the slitlets in spatial direction. Each slitlet was extracted and from there on treated like a long-slit spectrum. The flat fields were normalized with 4$^{\rm th}$ or 5$^{\rm th}$ order polynomials. The dispersion relation was obtained from the wavelength calibration frames by fitting 3$^{\rm rd}$ to 4$^{\rm th}$ order polynomials to the line positions along the dispersion axis. We used 13 to 16 unblended lines between 3600 Å and 6200 Å and achieved an r.m.s. error of 0.05 Å to 0.08 Å per row.

Due to exposure times of 2700 sec the scientific observations contained a large number of cosmic ray hits. Those were corrected with the algorithm described in Gössl & Riffeser ([@gori02]), using a threshold of 15$\sigma$ and a FWHM of 1.5 pixels for the cosmic ray hits. As the routine is not originally intended for the use with spectra, we also reduced the uncorrected frames to allow a check for any possible artifacts of the cosmic ray cleaning procedure. The slitlets with the stellar spectra were extracted in the same way as the flat field and wavelength calibration slitlets. The smoothed masterbias was subtracted, and the spectra were divided by the 