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In the planetary atmosphere, hydrogen cyanide (HCN) is an importantnitrogen-bearing molecule that plays a key role in the formation of severalbiomolecules via chain reactions. The presence of an HCN characterizes thestratospheric composition of the solar gas planets and exoplanets. For severalyears, many observations have failed to detect the emission lines of HCN fromthe atmosphere of Saturn using ground- and space-based radio telescopes. Wepresent the successful detection of the rotational emission line of HCN fromthe atmosphere of Saturn using the Atacama Large Millimeter/Submillimeter Array(ALMA) band 7. We detected the J = 4$-$3 transition line of the HCN from theeastern and western limbs of Saturn with $\geq$5$\sigma$ statisticalsignificance. The derived abundances of HCN in the western and eastern limbswere 6.19 ppb and 2.90 ppb, respectively. We claim that HCN was formed in theatmosphere of Saturn via the photolysis of methane (CH$_{4}$) and ammonia(NH$_{3}$).

ALMA detection of hydrogen cyanide (HCN) in the atmosphere of Saturn