Previous studies have identified carbon dioxide (CO₂) on the surfaces of Jovian and Galilean satellites in regions of non-ice material that are too warm for CO₂ ice to exist. CO₂ ice would quickly sublimate if not retained by a less-volatile material. To ascertain what non-ice species may be responsible for stabilizing this CO₂, we performed CO₂ gas adsorption experiments on thirteen powdered CM, CI, and CV carbonaceous chondrite meteorites. Reflectance spectra of the ν₃ feature associated with adsorbed CO₂ near 4.27 μm were recorded. Results show that many meteorites adsorbed some amount of CO₂, as evidenced by an absorption feature that was stable over several hours at ultra-high vacuum (UHV) and high vacuum, (1.0×10⁻⁸ and 1.0×10⁻⁷ Torr, respectively). Ivuna, the only CI chondrite studied, adsorbed significantly more CO₂ than the others. We found that CO₂ abundance did not vary with ‘water’ abundance, organics, or carbonates as inferred from the area of the 3-μm band, the 3.2-3.4 μm C-H feature, and the ∼3.8-μm band respectively, but did correlate with hydrous/anhydrous phyllosilicate ratios. Furthermore, we did not observe CO₂ ice because the position of the CO₂ feature was generally shifted 3-10 nm from that of the 4.27 μm absorption characteristic of ice. The strongest compositional relationship observed was a possible affinity of CO₂ for total FeO abundance and complex clay minerals, which make up the bulk of the CI chondrite matrix. This finding implies that the most primitive refractory materials in the Solar System may also act as reservoirs of CO₂, and possibly other volatiles, delivering them to parts of the Solar System where their ices would not be stable.