The method of galactic rotation distances is investigated by means of
numerical simulations and found to work properly, even when the disper
sion of the absolute magnitudes or the peculiar velocity dispersion ar
e large. We apply the method to a large sample of more than 600 galact
ic supergiants and bright giants. We derive average mean absolute magn
itudes which confirm the average absolute magnitudes found by either B
laauw or Schmidt-Kaler. Our calibration has the advantage to be based
upon both a single method and a large number of stars. We show that th
e method works properly only with large samples. Therefore no subdivis
ions according to spectral types can be derived. We show further that
the method is stable in the sense that small variations in the input p
arameters produce only small changes in the results.