The type parameter allows to select from a range of stellar models, either analytical, or available as data files or FITS images. Please note that a new numbering scheme was introduced with Version 6.12 (2 Aug 2007)
For all types from zero to 11, the flux distribution is computed as flat (teff=0), a black body (teff < 0), or a stellar atmosphere (teff > 0). For all types, specifying an arbitrary SED will override stellar spectra or fluxes derived from the images. The XDR file to read is specified in sed, and should restore variables and , which contain the wavelength in meters and the flux (per wavelength interval), respectively. Please note that if the effective of a component is non-zero, the flux will be scaled with the squared diameter! As mentioned above (readmodel), please keep in mind that an internal value of for an effective temperature is interpreted as zero.
In many models, specifying pa and ratio is used to rotate and stretch the coordinates. The only exceptions are the images if a positive non-zero diameter of the CLEAN beam have been specified.