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The milestone of GW 170817-GRB 170817A-AT 2017gfo has shown thatgravitational wave (GW) is produced during the merger of neutron star-neutronstar/black hole and that in electromagnetic (EM) wave a gamma-ray burst (GRB)and a kilonovae (KN) are generated in sequence after the merger.Observationally, however, EM property during a merger is still unclear. Here wereport a peculiar precursor in a KN-associated long GRB 211211A. The durationof the precursor is $\sim$ 0.2 s, and the waiting time between the precursorand the main emission (ME) of the burst is $\sim$ 1 s, which is about the sameas the time interval between GW 170817 and GRB 170817A. Quasi-PeriodicOscillations (QPO) with frequency $\sim$22 Hz (at $>5\sigma$ significance) arefound throughout the precursor, the first detection of periodic signals fromany {\it bona fide} GRBs. This indicates most likely that a magnetarparticipated in the merger, and the precursor might be produced due to acatastrophic flare accompanying with torsional or crustal oscillations of themagnetar. The strong seed magnetic field of $\sim 10^{14-15}$ G at the surfaceof the magnetar may also account for the prolonged duration of GRB 211211A.However, it is a challenge to reconcile the rather short lifetime of a magnetar\cite{kaspi2017magnetars} with the rather long spiraling time of a binaryneutron star system only by gravitational wave radiation before merger.

The quasi-periodically oscillating precursor of a long gamma-ray burst from a binary neutron star merger