We detected flaring flux variability that regularly occurred with the period of 23.9 days on a 6.7 GHz methanol maser emission at V _ { \mathrm { lsr } } = 25.30 km s ^ { -1 } in G 014.23 - 00.50 through highly frequent monitoring using the Hitachi 32-m radio telescope .
By analyzing data from 05 January 2013 to 21 January 2016 , the periodic variability has persisted in at least 47 cycles , corresponding to \sim 1,100 days .
The period of 23.9 days is the shortest one observed in masers at around high-mass young stellar objects so far .
The flaring component normally falls below the detection limit ( 3 \sigma ) of \sim 0.9 Jy .
In the flaring periods , the component rises above the detection limit with the ratio of the peak flux density more than 180 in comparison with a quiescent phase , showing intermittent periodic variability .
The time-scale of the flux rise was typically two days or shorter , and both symmetric and asymmetric profiles of flux variability were observed through intraday monitoring .
These characteristics might be explained by a change in the flux of seed photons by a colliding-wind binary ( CWB ) system or a variation of the dust temperature by an extra heating source of a shock formed by the CWB system within a gap region in a circumbinary disk , in which the orbital semi-major axes of the binary are 0.26–0.34 au .