Over a wide range of the tailward distances in the lobe/mantle regions (|XGSM'|≤210 RE), the Geotail spacecraft sometimes observed cold O+ beams (COBs) streaming tailward at a velocity nearly equal to that of the major proton component. The discovery of the ionospheric ions in the distant lobe/mantle leads us to a reexamination of the conventional view which expects these O+ ions to descend into the plasma sheet because of the E¿B drift. In order to clarify the quantitative property of the COBs, we have projected COB parameters onto the polar ionosphere with a simple model which takes into account the velocity filter effect alone. The statistical data set from October 1993 to March 1995 in a solar-minimum period is used in the calculation. The calculated average COB flux in the lobe/mantle corresponds to at least ~108 cm-2 s-1 O+ flux at the 1000-km altitude. From the comparison with polar outflows, it is suggested that the cusp/cleft originating O+ ions sometimes need significant additional energization(s) so as to supply the COBs in the distant tail. When we assume the typical flux and temperature of polar O+ outflows, the required bulk energy of upward flowing ions (UFIs) turns out to be of the order of 3 keV, which is much higher than the typical energy of cusp/cleft outflows (≤ 1 keV). The energy difference between the tail lobe/mantle and the cusp/cleft O+ provides clues to the supply and/or energization mechanisms of the ionospheric ions. Calculations with individual COB events suggest that the rate of COB events in which the ionospheric O+ outflow flux exceeds 109 cm-2 s-1 increases with the tailward distance, and it corresponds to 27% of all events in the distant tail of |XGSM'|≥150 RE. ¿ 1998 American Geophysical Union