Galactocentric distance dependences of the physical parameters of globular clusters. Notation is the same as in Fig. 3. The straight line in (a) is the rms regression. The large circles in (b) show mean masses within narrow R intervals, and the solid lines show the rms regression fits for thick-disk and old-halo (left) and young-halo and corona (right) clusters. The dashed lines in (c) and (d) are upper and lower envelopes drawn by eye.discussion in the text | privious figure | next figure