We have performed VLBI and single-dish monitoring of 22 GHz H _ { 2 } O maser emission from the high mass young stellar object G353.273+0.641 with VERA ( VLBI Exploration of Radio Astrometry ) and Tomakamai 11-m radio telescope . Two maser flares have been detected , separated almost two years . Frequent VLBI monitoring has revealed that these flare activities have been accompanied by structural change of the prominent shock front traced by H _ { 2 } O maser alignments . We have detected only blue-shifted emissions and all maser features have been distributed within very small area of 200 \times 200 au ^ { 2 } in spite of wide velocity range ( > 100 km s ^ { -1 } ) . The light curve shows notably intermittent variation and suggests that the H _ { 2 } O masers in G353.273+0.641 are excited by episodic radio jet . The time-scale of \sim 2 yr and characteristic velocity of \sim 500 km s ^ { -1 } also support this interpretation . Two isolated velocity components of C50 ( -53 \pm 7 km s ^ { -1 } ) and C70 ( -73 \pm 7 km s ^ { -1 } ) have shown synchronised linear acceleration of the flux weighted V _ { \mathrm { LSR } } values ( \sim -5 km s ^ { -1 } yr ^ { -1 } ) during the flare phase . This can be converted to the lower-limit momentum rate of 1.1 \times 10 ^ { -3 } M _ { \sun } km s ^ { -1 } yr ^ { -1 } . Maser properties are quite similar to that of IRAS 20126+4104 especially . This corroborates the previous suggestion that G353.273+0.641 is a candidate of high mass protostellar object . The possible pole-on geometry of disc-jet system can be suitable for direct imaging of the accretion disc in this case .