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Each of the nitriles present in the atmosphere of Titan can be expected toexhibit different \ce{^{14}N/^{15}N} values depending on their productionprocesses, primarily because of the various \ce{N2} dissociation processesinduced by different sources such as ultraviolet radiation, magnetosphericelectrons, and galactic cosmic rays. For \ce{CH3CN}, one photochemical modelpredicted a \ce{^{14}N/^{15}N} value as 120--130 in the lower stratosphere.This is much higher than that for \ce{HCN} and \ce{HC3N}, $\sim$67--94. Byanalyzing archival data obtained by the Atacama Large Millimeter/submillimeterArray (ALMA), we successfully detected submillimeter rotational transitions of\ce{CH3C^{15}N} ($J$ = 19--18) locate at the 338 GHz band in Titan'satmospheric spectra. By comparing those observations with the simultaneouslyobserved \ce{CH3CN} ($J$ = 19--18) lines at the 349 GHz band, which probe from160 to $\sim$400 km altitude, we then derived \ce{^{14}N/^{15}N} in \ce{CH3CN}as 125$^{+145}_{-44}$. Although the range of the derived value showsinsufficient accuracy due to data quality limitations, the best-fit valuesuggests that \ce{^{14}N/^{15}N} for \ce{CH3CN} is higher than values that havebeen previously observed and theoretically predicted for \ce{HCN} and\ce{HC3N}. This may be explained by the different \ce{N2} dissociation sourcesaccording to the altitudes, as suggested by a recent photochemical model.

$^{14}$N/$^{15}$N isotopic ratio in CH$_3$CN of Titan's atmosphere measured with ALMA