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Traditionally IVC and HVC were defined to be concentrations of HI gas, withline-of-sight velocities that are inconsistent with data on the differentialrotation of the Galaxy. We demonstrate that IVCs and HVCs can be identifiedfrom certain density enhancements in (V_C, FWHM) distribution of Gaussians,representing the Galactic HI 21 cm radio lines. We study the Gaussians, whichparameters fall into the regions of the phase-space density enhancements about$(V_C, FWHM) = (-131, 27), (164, 26) and (-49 km/s, 23 km/s). The skydistribution of the Gaussians, corresponding to the first two concentrations,very well represents the sky distribution of HVCs, as obtained on the basis ofthe traditional definition of these objects. The Gaussians of the lastconcentration correspond to IVCs. Based on this identification, the divisionline between IVCs and HVCs can be drawn at about |V_C| = 74 km/s, and IVCs canbe identified down to velocities of about |V_C| = 24 km/s. Traces of both IVCsand HVCs can also be seen in the sky distribution of Gaussians with FWHM = 7.3km/s. In HVCs, these cold cores have small angular dimensions and low observedbrightness temperatures T_b. In IVCs, the cores are both larger and brighter.This definition of IVCs and HVCs is less dependant than the traditional one, onthe differential rotation model of the Galaxy. The consideration of line-widthinformation may enable IVCs and HVCs to be better distinguished from eachother, and from the ordinary Galactic HI

Gaussian decomposition of HI surveys. IV. Galactic intermediate- and high-velocity clouds