The results of Ginga observations of the dipping X-ray source X1254-690 are presented. The persistent emission spectrum cannot be represented with conventional two-component models; an additional spectral structure, which can be represented either by a broad emission line or by reflection by warm matter, is required. The energy spectra during dips can be represented by the sum of a non-absorbed component, which has the same spectral shape as the persistent emissions just before or after the dip, and an absorbed component, which is described by the persistent spectrum with additional absorption. The intensity of the non-absorbed component first decreases with decreasing intensity; then, the decrease saturates at about 8% of the persistent intensity. This strongly supports the existence of an accretion-disk corona of an electron-scattering optical depth of about 0.1. The column density of the absorbed component obtained from spectral fit stays at about 1times 10(23) cm(-2) when the intensity of the non-absorbed component is above about 20% of the persistent intensity, but increases to 1 times 10(24) cm(-2) at the bottom of the dip. The electron-scattering optical depth of the accretion-disk corona and the column density of the absorber are roughly consistent with the double-phase model of X-ray irradiated accretion matter.