Spectroscopic detection of ethyl cyanide and water in the atmosphere of Jupiter using ALMA

Various trace species were detected for the first time in the atmosphere of Jupiter with the collision of comet Shoemaker-Levy 9 in July 1994 near 44$^\circ$ S. These trace species can be used to understand the chemical dynamics in the atmosphere of Jupiter. We present the first spectroscopic detection of the emission lines of ethyl cyanide (CH$_3$CH$_2$CN) in the atmosphere of Jupiter using the Atacama Large Millimeter/Submillimeter Array (ALMA). We detected five rotational emission lines of ethyl cyanide in the frequencies of 195.430, 195.722, 214.956, 231.296, 242.317 GHz with $\ge$4$\sigma$ significance. The column densities of ethyl cyanide emission lines are found in the range of (2-7)$\times$10$^{14}$ cm$^{-2}$ with exception of 195.722 GHz emission line. The column density of the ethyl cyanide emission line at 195.722 GHz is 5.26$\times$10$^{10}$ cm$^{-2}$. We also confirm the presence of water vapour in the atmosphere of Jupiter with the detection of the absorption line of water (H$_2$O) at frequency $\nu$ = 183.310 GHz ($\sim$4.3$\sigma$ statistical significance) with transition J = 3$_{1,3}$--2$_{2,2}$. The column density of water absorption line is N(H$_2$O)= 9.25$\times$10$^{14}$ cm$^{-2}$. We discussed possible photochemical pathways to produce detected ethyl cyanide in the atmosphere of Jupiter.