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We present results of the classification of cloud structures toward the OrionA Giant Molecular Cloud based on wide-field $^{12}$CO ($J$ = 1--0), $^{13}$CO($J$ = 1-0), and C$^{18}$O ($J$ = 1-0) observations using the Nobeyama 45 mradio telescope. We identified 78 clouds toward Orion A by applying SpectralClustering for Interstellar Molecular Emission Segmentation (SCIMES) to thedata cube of the column density of $^{13}$CO. Well-known subregions such asOMC-1, OMC-2/3, OMC-4, OMC-5, NGC 1977, L1641-N, and the dark lane southfilament (DLSF) are naturally identified as distinct structures in Orion A.These clouds can also be classified into three groups: the integral-shapedfilament, the southern regions of Orion A, and the other filamentary structuresin the outer parts of Orion A and the DLSF. These groups show differences inscaling relations between the physical properties of the clouds. We derived theabundance ratio between $^{13}$CO and C$^{18}$O,$X_{^{13}\mathrm{CO}}/X_{\mathrm{C}^{18}\mathrm{O}}$, which ranges from 5.6 to17.4 on median over the individual clouds. The significant variation of$X_{^{13}\mathrm{CO}}/X_{\mathrm{C}^{18}\mathrm{O}}$ is also seen within acloud in both of the spatial and velocity directions and the ratio tends to behigh at the edge of the cloud. The values of$X_{^{13}\mathrm{CO}}/X_{\mathrm{C}^{18}\mathrm{O}}$ decrease from 17 to 10with the median of the column densities of the clouds at the column density of$N_{\mathrm{C^{18}O}} \gtrsim 1 \times 10^{15}$ cm$^{-2}$ or visual extinctionof $A_V \gtrsim 3$ mag under the strong far-ultraviolet (FUV) environment of$G_0 > 10^{3}$, whereas it is almost independent of the column density in theweak FUV radiation field. These results are explained if the selectivephotodissociation of C$^{18}$O is enhanced under a strong FUV environment andit is suppressed in the dense part of the clouds.

publications of the astronomical society of japan

Nobeyama 45 m Mapping Observations toward Orion A. II. Classification of  cloud structures and variation of the $^{13}$CO/C$^{18}$O abundance ratio due  to far-UV Radiation