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Carbonaceous chondrites (CCs) are windows into the early Solar system and thehistories of their parent bodies. Their infrared spectral signatures arepowerful proxies for deciphering their composition and evolution history, butstill present formidable challenges. In our study, we delved into the infraredspectra spanning 1-25 micron of 17 CCs, with distinct petrologicalcharacteristics and varying degrees of alteration. As aqueous alterationintensifies, the 3 micron-region absorption feature associated with OH-bearingminerals and water, and the 6 micron band indicative of water molecules, bothgrow in intensity. Simultaneously, their band centers shift towards shorterwavelengths. Moreover, as alteration progresses, a distinctive absorptionfeature emerges near 2.72 micron, resembling the OH absorption feature found inserpentine and saponite minerals. Comparison of aqueous alteration tolaboratory-heated CCs suggests that the 3 micron region OH/H2O absorptionfeature differs between CC heated to less than or more than ~300C. The 12.4micron/11.4 micron reflectance ratio diminishes, and the reflectance peak inthe 9-14 micron range shifts towards shorter wavelengths. These changes areattributed to the transformation of anhydrous silicates into phyllosilicates.In the 15-25 micron region, the influence of thermal metamorphism becomesevident and results in the appearance of more spectral features, the singlereflectance peak at 22.1 micron undergoes a transformation into two distinctpeaks at 19 micron and 25 micron, which is primarily attributed to theincreased presence of anhydrous silicates and olivine recrystallization. Thesefindings offer novel insights into the volatile-rich compositions of C-complexasteroids and the thermal evolution histories of their parent bodies.

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Near-mid infrared spectroscopy of carbonaceous chondrites: Insights into  spectral variation due to aqueous alteration and thermal metamorphism in  asteroids