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tokens: configuration. 6. Formation of Molecular Gas Due to Jet–ISM Interactions? Figures 10 – 12 display that a wall structure is clearly seen toward the locus of the extension of the precession axis of the SS 433 jets, in which the column density of H i increased precipitously. Enhanced CO emissions are also found to be nicely associated with the wall structure seen in H i emission. MC G40.331−4.302 has the H i counterpart, which displays more extended arc-like structure nearly perpendicular to the precession axis of the SS 433 jets (Figure 12 ). The positional coincidence between G40.331−4.302 and the precession axis of SS 433, as well as their coincident kinematic features, strongly suggests the physical connection between them (see Sections 4 and 5 ). We obtain that the column density, N H = N (H i ) + 2 × N (H 2 ), is about 2.1 × 10 21 cm −2 for the cloud G40.331−4.302, which corresponds to A V ≈ 1.1 mag assuming N H ≈ 1.9 × 10 21 cm −2 mag −1 × A V . At the column density, the molecules are shielded from UV radiation, and self-shielding allows significant H 2 molecules to exist. The total mass of the main concentration of the cloud is ∼3 × 10 3 M ⊙ within a radius of ∼66 (Table 1 ). The molecular fraction / N H is about 0.87, suggesting that the dominant of the gas in the cloud is in molecular form. Table 1 Properties of Gas toward G39.315−1.155 and G40.331−4.302 Notes. a The area of the emission with I (CO)>5 K km s −1 for G39.315−1.155 and I (H i )>130 K km s −1 and I (CO)>2.5 K km s −1 for G40.331−4.302. b The effective radius is calculated from (Area/3.14) 0.5 . c The mean intensity of the H i (70–90 km s −1 ) and CO (73–88 km s −1 ) emission. d The column density of the atomic and molecular gas is calculated from 1.823 × 10 18 × I mean (H i ) and 2 × 10 20 × I mean (CO), respectively. See the text. e Parameter d 4.9 is the distance to the cloud in units of 4.9 kpc (see Section 4 ). f The volume density of the atomic and molecular gas is calculated from the mass and the effective radius of the emission. The virial mass exceeds the total mass of the cloud by more than one order of magnitude, indicating that the cloud is in a gravitationally unbound state. The fragmented subclouds (e.g., with a size of ∼1 pc) in MC G40.331−4.302 may dissipate on a timescale of several Myr (sound crossing time) without other support. Alternatively, the MC may be confined by an external pressure of ≳4.4 × 10 4 K cm −3 (e.g., ρ (H i ) σ 2 (H i )) when the magnetic pressure and the self-gravity are negligible. We emphasize that G40.331−4.302 is the only detected MC within the range of l = 349–451, −51 ≲ b ≲ −30, and V LSR ≳ 70 km s −1 . It indicates that such an MC is located about 370 pc below the Galactic plane, where a kinematic distance of 4.9 kpc is adopted. However, the MCs within the solar circle are concentrated in the Galactic plane with a Gaussian FWHM of ∼90–100 pc (e.g., see Section 4.5 and Figure 6 in Heyer Dame 2015 ). This suggests that