Description

Read-noise and Poisson variances are added to the frame and a bad pixel mask is applied. The spectrum from each slice of the IFU is cut out of the frame and pasted in a new frame in such a way that there are no longer spaces between the spectra, the spectra are arranged in the order in which they appear in the field of view and they are approximately aligned in the dispersion direction. The spectrum is flat-fielded and sky-object pairs are now subtracted. The wavelength calibration previously measured from the arc spectrum is used to apply a common, linear wavelength scale to each row of the the sky-subtracted 2-d spectrum. The resulting frame is coadded to the group, which is then rearranged to form a data-cube. The spectral dimension of the data-cube is divided by the standard-star spectrum and flux calibrated. Images can be extracted over a range of wavelengths specified in a file called extract.images placed in the $ORAC_DATA_OUT directory, and can be displayed by editing the disp.dat file.