\relax 
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Enclosed mass vs radius}}{4}}
\newlabel{fig:theta}{{1}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Rotation curve, the filled circle is at $r=8.5{\hbox {\rm  kpc}}$, $V_c=220{\hbox {\rm  km s$^{-1}$}}$. There is Keplerian fall-off $V_c\propto 1/r^{1/2}$ both very close to the black hole (where it dominates the mass), and on large scales $r\ge r_2$, where the galaxy mass is constant. In the inner region, where the mass is dominated by the $1/r$ density profile, the circular velocity rises, $V_c\propto r^{1/2}$, and where the $1/r^2$ density dominates the mass, the circular velocity becomes almost constant, $V_c\approx 220{\hbox {\rm  km s$^{-1}$}}$. The short dashed line is the Keplerian fall-off due to the black hole, the long-dashed is the Keplerian fall-off due to the $1/r$ density distribution. The open circle is where we computed that the black hole started contributing significantly to $V_c$.}}{5}}
\newlabel{fig:theta}{{2}{5}}