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Fragments of small solar system bodies entering Earth's atmosphere havepossibly been important contributors of organic compounds to the early Earth.The cyano radical (CN) emission from meteors is considered as potentially oneof the most suitable markers of organic compounds in meteoroids, however, itsdetection in meteor spectra has been thus far unsuccessful. With the aim toimprove our abilities to identify CN emission in meteor observations and useits spectral features to characterize the composition of incoming asteroidalmeteoroids, we present a detailed analysis of CN emission from high-resolutionspectra of 22 laboratory simulated meteors including ordinary, carbonaceous,and enstatite chondrites, as well as a large diversity of achondrites (i.e.,ureilite, aubrite, lunar, martian, howardite, eucrite, and diogenite),mesosiderite, and iron meteorites. We describe the variations of CN emissionfrom different classes of asteroidal meteor analogues, its correlation and timeevolution relative to other major meteoroid components. We demonstrate that CNcan be used as a diagnostic spectral feature of carbonaceous and carbon-richmeteoroids, while most ordinary chondrites show no signs of CN. Our resultspoint out strong correlation between CN and H emission and suggest bothvolatile features are suitable to trace contents of organic matter and watermolecules present within meteoroids. For the application in lower resolutionmeteor observations, we demonstrate that CN can be best recognized in the earlystages of ablation and for carbon-rich materials by measuring relativeintensity ratio of CN band peak to the nearby Fe I-4 lines.

Analysis of CN emission as a marker of organic compounds in meteoroids using laboratory simulated meteors