UV coronal intensity data collected by the Ultraviolet Coronagraph
Spectrometer on SOHO in a daily synoptic program during the Whole Sun
Month are used to reconstruct the 3D distribution of emissivities in the
solar corona for H I Ly-alpha and the O VI doublet at 1032 and 1037
angstroms.  We discuss the specifics that complicate a tomographic
reconstruction of the solar corona and estimate the uncertainties
introduced in the reconstruction by them.