Carbonaceous chondrites are one of the most primitive substances in the solar system. Through the spectral analysis of carbonaceous chondrites, the relationship between them and the parent asteroid can be established, which is helpful to analyze the composition of the surface of the asteroid and the early evolutionary history of the solar system. In this paper, the relationship between the visible-far infrared reflectance spectra of 6 CM2 carbonaceous chondritesand and 11 coal samples (earth analogs of organic matter contained in carbonaceous chondrites) and their organic components was studied. The results of the study show that for different types of coal samples, as the degree of coalification increases, the depth of the absorption peak of each organic hydrocarbon group continues to decrease. The depth of aliphatic hydrocarbons at 3.41 μm was linearly positive correlated with the H/C ratio, when the H/C ratio was less than 0.55, there was no obvious spectral characteristic at 3.41 μm. In the 3-4 μm region, the CM2 meteorites have obvious aliphatic CH2 and CH3 absorption, lacking 3.28 μm aromatic CH absorption, but in the 5--6.5 μm region, there are weak aromatic C=C and CO absorption. This indicates that the organic components of CM2 carbonaceous chondrites contain aliphatic and aromatic groups. The spectral features of the 3.28 μm and 5--6.5 μm regions of the meteorite are not obvious, which may be due to the overlapping absorption of water-bearing mineral OH in this band or the influence of other opaque minerals, the specific reasons for which need to be further studied. This study also indicates that a longer band range is needed to reliably identify the organic matter types of asteroids.