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The low mass protostar IRAS 16293$-$2422 is a well-known young stellar systemthat is observed in the L1689N molecular cloud in the constellation ofOphiuchus. In the interstellar medium and solar system bodies, water is anecessary species for the formation of life. We present the spectroscopicdetection of the rotational emission line of water (H$_{2}$O) vapour from thelow mass protostar IRAS 16293$-$2422 using the Atacama LargeMillimeter/submillimeter Array (ALMA) band 5 observation. The emission line ofH$_{2}$O is detected at frequency $\nu$ = 183.310 GHz with transitionJ=3$_{1,3}$$-$2$_{2,2}$. The statistical column density of the emission line ofwater vapour is $N$(H$_{2}$O) = 4.2$\times$10$^{16}$ cm$^{-2}$ with excitationtemperature ($T_{ex}$) = 124$\pm$10 K. The fractional abundance of H$_{2}$Owith respect to H$_{2}$ is 1.44$\times$10$^{-7}$ where $N$(H$_{2}$) =2.9$\times$10$^{23}$ cm$^{-2}$.

ALMA detection of water vapour in the low mass protostar IRAS 16293$-$2422