ON THE KEPLERIAN ROTATION CURVES OF GALAXIES

We propose a criterion for examining whether or not the uncertainty of the outer rotation curves is sufficiently small to distinguish a Kepl erian rotation curve from flat ones. We have applied this criterion to both Keplerian and non-Keplerian rotation curves so far obtained, and investigated their relative fraction. We also studied the minimum ext ent of the dark halos indicated by non-Keplerian rotation curves using the criterion. We have found that one cannot rule out the possibility that a significant fraction of rotation curves become Keplerian withi n 10-times the disk scale length. If the Keplerian rotation curves so far observed trace the mass truncation, several galaxies may have rath er small halos, the extent of which is not larger than twice that of t he optical disk.