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Stellar models

The code parameter allows to select from a range of stellar models, either analytical, or availbale as data files or FITS images. Please note that a new numbering scheme was introduced with Version 6.12 (2 Aug 2007)

For all codes 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 codes, specifying an arbitrary SED will override stellar spectra or fluxes derived from the images. The XDR file is given in sed, and should restore variables $l$ and $f$, which contain the wavelength in meters and the flux (per wavelength interval), respectively.

In many models, specifying pa and ratio is used to rotate and stretch the $(u,v)$ coordinates. The only exceptions are the images if a positive non-zero diameter of the CLEAN beam have been specified.



Subsections

Christian Hummel 2009-10-20