  Classical Cepheids are useful tracers of the Galactic young stellar
population because their distances and ages can be determined from their
period-luminosity and period-age relations. In addition, the radial velocities
and chemical abundance of the Cepheids can be derived from spectroscopic
observations, providing further insights into the structure and evolution of
the Galaxy. Here, we report the radial velocities of classical Cepheids near
the Galactic Center, three of which were reported in 2011, the other reported
for the first time. The velocities of these Cepheids suggest that the stars
orbit within the Nuclear Stellar Disk, a group of stars and interstellar matter
occupying a region of 200 pc around the Center, although the three-dimensional
velocities cannot be determined until the proper motions are known. According
to our simulation, these four Cepheids formed within the Nuclear Stellar Disk
like younger stars and stellar clusters therein.
