  Dark matter with MeV scale mass is difficult to detect with standard direct
search detectors. However, they can be searched for by considering the
up-scattering of kinetic energies by cosmic rays. Because the dark matter
density is higher in the central region of the Galaxy, the up-scattered dark
matter will arrive at Earth from the direction of the Galactic center. Once the
dark matter is detected, we can expect to recognize this feature by directional
direct detection experiments. In this study, we simulate the nuclear recoils of
the up-scattered dark matter and quantitatively reveal that a large amount of
this type of dark matter is arriving from the direction of the Galactic center.
Also, we have shown that the characteristic signatures of the up-scattered dark
matter can be verified with more than 5$\sigma$ confidence levels for the
assumed target atoms and future upgrades to directional detectors.
