The main output data product produced during EXTRACT is the high-dispersion MX FITS file (MXHI). The MXHI contains the net (background-subtracted) integrated flux spectrum, the Chebyshev-characterized background spectrum scaled up to the extraction slit area, the flag spectrum, the ripple-corrected spectrum, the absolutely-calibrated and ripple-corrected net flux spectrum, and the noise spectrum stored in a FITS binary table extension. The net flux, background, ripple, and noise spectra are in units of FN, the flag spectrum is in bit-encoded unitless values, and the calibrated flux spectrum is in physical units of ergs sec-1 cm-2 Å-1. See Chapter 11 for details concerning the process of absolute flux calibration and ripple correction.
The background values for locations before the short-wavelength ends or past the long-wavelength ends of the orders are replications of the first (or last) valid background value. The net flux and noise spectra are computed over the entire wavelength space of the high-dispersion SI, but locations that are outside the camera target area will have net fluxes equal to zero because these regions do not contain any valid image data. The absolute calibrations are valid over wavelength limits of 1150-1980Å for SWP and 1850-3350Å for LWP and LWR. Beyond these limits the calibrated net fluxes are set to a value of 0 and and have a flag value of -2. The valid wavelength limits of the calibrated spectra are consequently somewhat truncated as compared to the net flux spectrum.
The EXTRACT module writes the following information to the HISTORY portion of the image label: