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The purpose of the SOLIS Zeemanfit Code is to provide a straight-forward,easily checked measure of the total magnetic-field strength in thehigh-strength umbral regions of the solar disk. In the highest-strengthregions, the Zeeman splitting of the 6302-angstrom Fe line becomes wide enoughfor the triplet nature of the line to be visible by eye in non-polarized light.Therefore, a three-line fit to the spectra should, in principle, provide afairly robust measure of the total magnetic-field strength.  The code uses the Level-1.5 spec-cube data of the SOLIS VSM 6302-vectorobservations (specifically the Stokes-I and Stokes-V components) to fit theline profiles at each appropriate pixel and calculate themagnetic-field-strength from the line-center separation of the two fit 6302.5sigma-components. The 6301.5-angstrom Fe line is also present and fit in theVSM 6302-vector data, but it is an anomalous-Zeeman line with a weaker responseto magnetic fields. Therefore, no magnetic- field measure is derived from thisportion of the spectral fit.

Zeemanfit: Use and Development of the solis_vms_zeemanfit code