The repeating fast radio burst (FRB) source that produced FRB 121102 was recently localized in a star forming galaxy at $z=0.193$, which is associated with an extended radio source at the burst location. One possibility is that the repeating FRBs are produced by a new-born magnetar, which also powers the radio nebula. If so, the magnetar may produce $\gamma$-ray emission due to magnetic dipolar spin-down. The luminosity depends on the magnetar spin parameters and age. We process the eight-year Fermi LAT data at the position of FRB 121102 and place an energy flux upper limit of $\sim 10^{ -11} \ { \rm erg \ cm^{ -2} \ s^{ -1}}$ in time bins with six-month intervals, and an accumulated energy flux upper limit of $\sim 4\times 10^{ -12} \ { \rm erg \ cm^{ -2} \ s^{ -1}}$ over the eight year span. The corresponding $\gamma$-ray luminosity upper limits are $\sim 10^{ 45} \ { \rm erg \ s^{ -1}}$ and $\sim 4\times 10^{ 44} \ { \rm erg \ s^{ -1}}$ for the time-resolved and time-integrated analyses, respectively. We discuss the implications of these limits on the young magnetar model.
Categories: astro-ph.HE