The rotation curve of the Large Magellanic Cloud, which we have derived from
high-resolution HI position-velocity diagrams observed by Kim et al (1998),
shows a steep central rise and flat rotation with a gradual rise toward the
edge. Using the rotation curve, we have calculated the distribution of surface
mass density, and show that the LMC has a dark compact bulge, an exponential
disk, and a massive halo. The bulge is 1.2 kpc away from the center of the
stellar bar, and is not associated with an optical counterpart. This indicates
that the "dark bulge" has a large fraction of dark matter, with an anomalously
high mass-to-luminosity (M/L) ratio. On the contrary, the stellar bar has a
smaller M/L ratio compared to the surrounding regions.
(http://www.ioa.s.u-tokyo.ac.jp/~sofue/99lmc.htm)Comment: PASJ 1999 in press, Latex with Postscript figure
