- intermediate: *_str.fits, 2D images with orders straightened and bad pixel removed
- final output: *_e2ds.fits. The spectra are flat-fielded, extracted, calibrated, and the cosmic rays are removed. The echelle orders are not merged. The FITS files contain three images 50 orders x 2048 pixels: the primary image contains the fluxes, the second contains the wavelength calibration and the third contains the signal-to-noise ratio.
- final output: *_ms1d.fits. The spectra are flat-fielded, extracted, calibrated, and the cosmic rays are removed. The echelle orders are not merged. The FITS table has 50 rows and 4 columns, and it stores each echelle order in a row. The columns are: the number of the echelle order (from 32 - the reddest - to 81 - the bluest), the wavelength in nanometers, the fluxes and the signal-to-noise ratios.
- final output (optional): *_s1d.fits. The spectra are flat-fielded, extracted, calibrated, and the cosmic rays are removed. The echelle orders are merged. The barycentric correction is applied. These are monodimensional spectra with constant step in wavelength.