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In the Jovian atmosphere, the trace species are detected for the first timeafter the collision of comet Shoemaker-Levy 9 near 44$^\circ$S in July 1994.Most of these trace species are detected with spectroscopicmillimeter/submillimeter observation. In the atmosphere of Jupiter, trace gasesplay an important role in atmospheric chemistry with heterogeneous andhomogeneous chemical reactions, interaction with radiation, and phasetransition. Here we present the first spectroscopic detection of the rotationalemission line of water (H$_{2}$O) in the atmosphere of Jupiter at frequency$\nu$ = 183.310 GHz with molecular transition J = 3$_{1,3}$$-$2$_{2,2}$ usingAtacama Large Millimeter/Submillimeter Array (ALMA). The statistical columndensity of water emission line is N(H$_{2}$O)$\sim$4$\times$10$^{15}$cm$^{-2}$. The rotational emission line of H$_{2}$O is found in thestratosphere of Jupiter with $\geq$3$\sigma$ statistical significance. Thecolumn density of H$_{2}$O corresponds to the fractional abundance relative toH$_{2}$ is f(H$_{2}$O)$\sim$ 4$\times$10$^{-9}$.

ALMA spectroscopic detection of water vapour in the atmosphere of the giant gas planet Jupiter